pith. sign in

arxiv: 2605.28715 · v1 · pith:7NAMRWZUnew · submitted 2026-05-27 · 🌀 gr-qc · astro-ph.HE

Accurate waveforms for generic planar-orbit binary black holes: The multipolar effective-one-body model SEOBNRv6EHM

Aldo Gamboa , Alessandra Buonanno , Lorenzo Pompili , Raffi Enficiaud , Michael Boyle , Lawrence E. Kidder , Oliver Long , Peter James Nee
show 3 more authors
Harald P. Pfeiffer Antoni Ramos-Buades Mark A. Scheel
This is my paper

Pith reviewed 2026-06-29 10:37 UTC · model grok-4.3

classification 🌀 gr-qc astro-ph.HE
keywords binary black holesgravitational waveformseccentric orbitseffective one bodynumerical relativitymultipolar modesdynamical captures
0
0 comments X

The pith

SEOBNRv6EHM produces accurate multipolar waveforms for binary black holes on generic planar orbits with mismatches under 2 percent even at high eccentricity.

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

The paper introduces SEOBNRv6EHM, a time-domain multipolar effective-one-body waveform model for binary black holes on generic planar orbits. It extends previous models by incorporating novel resummations of the radiation-reaction force and waveform modes, calibrated only to quasi-circular numerical relativity simulations. The model includes several higher-order multipoles and is shown to achieve mismatches below or close to 2 percent for eccentricities up to approximately 0.9 in systems with total masses between 20 and 200 solar masses. This accuracy holds even for systems with 14 periastron passages before merger, and the model is faster to generate than comparable eccentric EOB models. Such performance matters because eccentricity is a signature of dynamical formation channels in gravitational wave observations.

Core claim

SEOBNRv6EHM is built within the effective-one-body framework and employs novel resummations of the radiation-reaction force and waveform modes. Validated against 592 quasi-circular, 319 eccentric, one dynamical-capture, and two scattering SXS NR waveforms, as well as scattering-angle comparisons, it attains unprecedented accuracy for highly eccentric systems with waveform mismatches remaining below or close to 2 percent across the total mass range 20-200 solar masses for eccentricities up to approximately 0.9 at 14 periastron passages before merger. It also achieves waveform-generation walltimes that are 2-6 times faster than other state-of-the-art EOB eccentric models.

What carries the argument

The multipolar effective-one-body framework with novel resummations of the radiation-reaction force and waveform modes, calibrated to quasi-circular numerical relativity simulations.

If this is right

  • Waveform mismatches remain below or close to 2 percent for highly eccentric systems up to eccentricity 0.9 across total masses 20-200 solar masses.
  • The model covers the full inspiral-merger-ringdown for dynamical captures and scattering encounters in addition to bound orbits.
  • Higher multipoles including (2,1), (3,3), (3,2), (4,4), and (4,3) are provided alongside the dominant (2,2) mode.
  • Waveform generation is 2-6 times faster than other state-of-the-art eccentric EOB models.
  • Accuracy remains comparable to previous-generation SEOBNRv5 models for quasi-circular and small-eccentricity cases.

Where Pith is reading between the lines

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

  • Better handling of eccentricity could reduce systematic biases when inferring parameters of binaries formed through dynamical channels in dense environments.
  • The speed gain might enable broader use of eccentric templates in large-scale gravitational wave searches and population studies.
  • The resummation techniques could be tested for extension to spinning or non-planar configurations in follow-up work.

Load-bearing premise

The novel resummations developed and calibrated primarily for quasi-circular orbits remain accurate when applied to highly eccentric orbits and dynamical captures without further tuning.

What would settle it

A numerical relativity simulation of an eccentric binary with eccentricity near 0.9 and 14 periastron passages before merger that produces a mismatch exceeding 2 percent when compared to SEOBNRv6EHM would falsify the accuracy claim.

Figures

Figures reproduced from arXiv: 2605.28715 by Aldo Gamboa, Alessandra Buonanno, Antoni Ramos-Buades, Harald P. Pfeiffer, Lawrence E. Kidder, Lorenzo Pompili, Mark A. Scheel, Michael Boyle, Oliver Long, Peter James Nee, Raffi Enficiaud.

Figure 1
Figure 1. Figure 1: EOB dynamics (left panels) and the associated GW emission (right panels), both in geometric units, for di [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Evolution of the functions dϕ = dϕ(r,r˙, p˙r∗,cons; α) (left panels) and dr = dr(r,r˙, p˙r∗,cons; α, β) (right panels), defined in Eqs. (46), for different values of the leading-order RR gauge constants α and β. Each row corresponds to a fixed value of α, while β is varied over the interval [−7, 7], as indicated by the color bars. Dashed curves indicate specific gauge choices, including the one used in SEO… view at source ↗
Figure 3
Figure 3. Figure 3: Top panel: Uniform distribution in mean anomaly and its mapping to relativistic anomaly through Eqs. (51) and (52). Bottom panel: Uniform distribution in relativistic anomaly and its mapping to mean anomaly through Eqs. (51) and (54). Both uniform distribu￾tions are composed of 107 random samples over the interval [0, 2π]. The mappings are performed at an eccentricity of 0.3. B. Generic planar orbits We de… view at source ↗
Figure 4
Figure 4. Figure 4: Parameter-space distribution of the 592 QC [PITH_FULL_IMAGE:figures/full_fig_p019_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Relative velocity (top panel) and separation (bottom panel) [PITH_FULL_IMAGE:figures/full_fig_p024_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Waveform mismatches between different approximants and the 592 QC SXS NR simulations used in this work, computed over the total mass range M ∈ [10, 300] M⊙. Nonspinning cases are shown in orange and spinning cases in blue. Columns 1–3 correspond to SEOBNRv5EHM, SEOBNRv6EHM, and TEOBResumS-Dal´ı, respectively. The top panels show the (2, 2)-mode mismatch M22, while the bottom panels display the sky-and-pola… view at source ↗
Figure 8
Figure 8. Figure 8: Distribution of maximum mode-by-mode mismatches be [PITH_FULL_IMAGE:figures/full_fig_p026_8.png] view at source ↗
Figure 7
Figure 7. Figure 7: Histograms of SNR-weighted mismatches, maximized [PITH_FULL_IMAGE:figures/full_fig_p026_7.png] view at source ↗
Figure 9
Figure 9. Figure 9: Parameter-space distribution of the 319 eccentric [PITH_FULL_IMAGE:figures/full_fig_p027_9.png] view at source ↗
Figure 11
Figure 11. Figure 11: Waveform mismatches between different approximants and the 319 eccentric SXS NR simulations used in this work, computed over the total mass range M ∈ [20, 200] M⊙. Curve color represents the earliest GW eccentricity egw of each NR waveform measured by gw eccentricity. Nonspinning cases are shown with solid curves, and spinning cases with dashed curves. Columns 1–3 correspond to SEOBNRv5EHM, SEOBNRv6EHM, a… view at source ↗
Figure 12
Figure 12. Figure 12: Top panels: Distributions of the maximum (purple), median (green), and minimum (yellow) (2, 2)-mode mismatches M22 (left) and sky-and-polarization-averaged, SNR-weighted mismatches MSNR (right) over the total mass range M ∈ [20, 200] M⊙, for different waveform models against the 319 eccentric SXS NR waveforms employed in this work. The horizontal lines represent the corresponding medians of the maximum, m… view at source ↗
Figure 13
Figure 13. Figure 13: Real parts and amplitudes of the waveform modes for a highly eccentric, equal-mass, nonspinning BBH, shown in geomet [PITH_FULL_IMAGE:figures/full_fig_p030_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: Mismatch between NR waveforms with only the (2 [PITH_FULL_IMAGE:figures/full_fig_p031_14.png] view at source ↗
Figure 15
Figure 15. Figure 15: Real part and amplitude of the waveform modes for [PITH_FULL_IMAGE:figures/full_fig_p033_15.png] view at source ↗
Figure 16
Figure 16. Figure 16: Scattering angles θ for six sets of binary configurations as functions of mass ratio, spins, energy E/M, reduced orbital angular momentum L/(µM), effective energy γ, and impact parameter b/M. Data are extracted from NR simulations [381] (black dots with error bars) and compared with the predictions of SEOBNRv5HM (blue), SEOBNRv6EHM (red), and TEOBResumS-Dal´ı (yellow); vertical dotted lines mark the first… view at source ↗
Figure 17
Figure 17. Figure 17: Walltime for waveform generation of SEOBNRv5HM (dashed), SEOBNRv5PHM (dash-dotted), SEOBNRv5EHM (solid-dotted), and SEOBNRv6EHM (solid), as function of the total mass M ∈ [5, 100] M⊙. The systems are characterized by a starting orbit-averaged frequency ⟨fstart⟩ = 10 Hz, dimensionless spin com￾ponents χ1 = 0.8 and χ2 = 0.3, and three different mass ratios q ∈ {1, 3, 10}. For SEOBNRv5EHM and SEOBNRv6EHM, th… view at source ↗
Figure 18
Figure 18. Figure 18: Histograms of waveform-evaluation walltimes for di [PITH_FULL_IMAGE:figures/full_fig_p036_18.png] view at source ↗
Figure 19
Figure 19. Figure 19: Contour plots of the initial separation as a function of the [PITH_FULL_IMAGE:figures/full_fig_p037_19.png] view at source ↗
Figure 20
Figure 20. Figure 20: Uniform variation of eccentricity (left panels), relativistic anomaly (middle panels), and mean anomaly (right panels) for the [PITH_FULL_IMAGE:figures/full_fig_p039_20.png] view at source ↗
Figure 21
Figure 21. Figure 21: Variation of the GW polarizations, h+ and h× (in geometric units), with respect to the energy E/M (top panel) and total angular momentum J/M2 (bottom panel), as predicted by SEOBNRv6EHM. Each of these waveforms belongs to a BBH system with mass ratio q = 3, dimensionless spin components χ1 = 0.3 and χ2 = −0.4, initial separation r = 500M, and a line-of-sight inclination of ι = π/3. The specific energy val… view at source ↗
Figure 22
Figure 22. Figure 22: Fits for the a6 (left panel) and ∆t 22 ISCO, noS (right panel) calibration parameters, as functions of the symmetric mass ratio ν. The fits are given by Eqs. (B1) and (B3b), respectively, and are obtained by least-squares regression of the maximum-likelihood values (max L, blue dots) of the calibration posteriors (shaded violins) for a set of 21 QC SXS NR simulations, including test-mass limit estimates (… view at source ↗
Figure 23
Figure 23. Figure 23: Fits for the dˆ SO (left plot) and ∆t 22 ISCO (right plot) calibration parameters, as functions of the spin variables a+ and a−. The fits are given by Eqs. (B2b) and (B3a)–(B3c), respectively, and are obtained by least-squares regression of the median values (blue dots) of the calibration posteriors (shaded violins) for a set of 78 QC, equal-mass SXS NR simulations. In the right panels, a dashed horizonta… view at source ↗
read the original abstract

Accurate and computationally efficient waveform models are required to infer the parameters of compact binaries from their gravitational wave (GW) emission. Among these parameters, orbital eccentricity serves as a smoking gun for dynamical formation channels and must be accounted for to avoid systematic errors in GW analyses. Here, we present SEOBNRv6EHM, a time-domain, multipolar waveform model for binaries on generic planar orbits, calibrated to quasi-circular (QC) numerical-relativity (NR) simulations from the SXS collaboration. In addition to the dominant $(2,2)$ mode, the model provides the $(2,1)$, $(3,3)$, $(3,2)$, $(4,4)$, and $(4,3)$ multipoles for the full inspiral-merger-ringdown process of coalescing binaries, as well as for dynamical captures and scattering encounters. The model is built within the effective-one-body (EOB) framework, and it employs novel resummations of the radiation-reaction force and waveform modes. We validate its accuracy through comparisons against 592 QC, 319 eccentric, one dynamical-capture, and two scattering SXS NR waveforms, and through scattering-angle comparisons against 61 SXS NR simulations. For QC and small-eccentricity binaries, its accuracy is comparable to previous-generation SEOBNRv5 models. For highly eccentric systems, however, SEOBNRv6EHM attains unprecedented accuracy, with waveform mismatches remaining below or close to $ 2\% $ across the total mass range $ 20-200\, \mathrm{M}_\odot $ for eccentricities up to $\sim 0.9$ at 14 periastron passages before merger. Additionally, SEOBNRv6EHM achieves waveform-generation walltimes that are $ 2 - 6 $ times faster than other state-of-the-art EOB eccentric models, enabling efficient and accurate applications in GW astronomy.

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

0 major / 2 minor

Summary. The manuscript introduces SEOBNRv6EHM, a time-domain multipolar effective-one-body waveform model for generic planar orbits of binary black holes. It is calibrated to quasi-circular SXS NR simulations and provides the (2,2), (2,1), (3,3), (3,2), (4,4), and (4,3) modes for inspiral-merger-ringdown, dynamical captures, and scattering encounters. The central claim is that the model achieves mismatches below or close to 2% against 319 eccentric SXS NR waveforms (plus 592 QC, one capture, and two scattering cases) for eccentricities up to ~0.9 at 14 periastron passages, while being 2-6 times faster than prior eccentric EOB models.

Significance. If the reported accuracy holds, the model would be significant for gravitational-wave astronomy by enabling reliable parameter estimation for eccentric binaries, which serve as indicators of dynamical formation channels. The direct validation against 319 eccentric NR waveforms (rather than extrapolation) provides empirical grounding for the performance on highly eccentric orbits. Credit is given for the scale of the NR comparison set and the reported computational speedup, both of which strengthen the practical utility of the result.

minor comments (2)
  1. The abstract states mismatches remain below or close to 2% across 20-200 M_⊙ for e up to ~0.9, but the main text should explicitly define the mismatch measure (e.g., which modes are included, frequency range, and noise curve) and report the distribution of mismatches rather than only the upper bound.
  2. The description of the novel resummations of the radiation-reaction force and waveform modes would benefit from a dedicated subsection or appendix that isolates their functional form and shows how they reduce to the quasi-circular limit.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for the positive assessment of SEOBNRv6EHM, the recognition of its potential impact for eccentric binary parameter estimation, and the recommendation for minor revision. We appreciate the credit given to the scale of the NR validation set and the reported computational performance.

Circularity Check

0 steps flagged

No significant circularity

full rationale

The model is calibrated exclusively to quasi-circular SXS NR simulations and then validated by direct mismatch comparisons against an independent set of 319 eccentric SXS NR waveforms (plus capture and scattering cases) that were not used in the fit. The reported accuracy for e up to ~0.9 is therefore an empirical test rather than a quantity forced by the calibration inputs. No self-definitional equations, fitted-input-called-prediction steps, or load-bearing self-citation chains that reduce the central claim to its own inputs appear in the provided text; the EOB resummations are applied within an existing framework whose eccentric dynamics are already defined independently of the validation data.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

Ledger constructed from abstract description; specific free parameters and axioms not enumerated in the provided text.

free parameters (1)
  • EOB calibration parameters
    Parameters fitted to match quasi-circular NR simulations from SXS collaboration.
axioms (1)
  • domain assumption Effective-one-body framework provides an accurate mapping for two-body dynamics in general relativity
    Fundamental to the construction of the SEOBNR models.

pith-pipeline@v0.9.1-grok · 5932 in / 1270 out tokens · 44937 ms · 2026-06-29T10:37:14.891808+00:00 · methodology

discussion (0)

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

Forward citations

Cited by 3 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. Joint inference of line-of-sight acceleration and orbital eccentricity in neutron-star--black-hole binaries

    gr-qc 2026-06 unverdicted novelty 7.0

    All five NSBH events are consistent with zero line-of-sight acceleration; the joint posterior for GW200105_162426 disfavors both zero LOSA and zero eccentricity at 90% credibility.

  2. Horizon absorption in eccentric precessing binary black hole inspirals and its importance for gravitational wave data analysis

    gr-qc 2026-06 unverdicted novelty 7.0

    First leading-PN derivation of horizon absorption in eccentric precessing BBH inspirals, incorporated into pyEFPEHM, with estimates showing parameter biases in eccentric systems at moderate SNR.

  3. Weak-field waveforms for generic relativistic orbits

    hep-th 2026-06 unverdicted novelty 5.0

    Outlines a Schwinger-Keldysh path-integral framework that derives worldline equations of motion and computes weak-field gravitational waveforms independently for unspecified relativistic orbits.

Reference graph

Works this paper leans on

300 extracted references · 275 canonical work pages · cited by 3 Pith papers · 102 internal anchors

  1. [1]

    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

  2. [2]

    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: Com- pact Binary Coalescences Observed by LIGO and Virgo Dur- ing the First Half of the Third Observing Run, Phys. Rev. X 11, 021053 (2021), arXiv:2010.14527 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2021

  3. [3]

    R. Abbottet al.(LIGO Scientific, VIRGO), GWTC-2.1: Deep Extended Catalog of Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observ- ing Run, Phys. Rev. D109, 022001 (2024), arXiv:2108.01045 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2024

  4. [4]

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

    R. Abbottet al.(LIGO Scientific, VIRGO, KAGRA), 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. [5]

    GWTC-4.0: Updating the Gravitational-Wave Transient Cata- log with Observations from the First Part of the Fourth LIGO- Virgo-KAGRA Observing Run, (2025), arXiv:2508.18082 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  6. [6]

    GWTC-4.0: Population Properties of Merging Compact Bina- ries, (2025), arXiv:2508.18083 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  7. [7]

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

    1963

  8. [8]

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

    1964

  9. [9]

    Circularization and Final Spin in Eccentric Binary Black Hole Inspirals

    I. Hinder, B. Vaishnav, F. Herrmann, D. Shoemaker, and P. La- guna, 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

  10. [10]

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

    U. Sperhake, E. Berti, V . Cardoso, J. A. Gonzalez, B. Brueg- mann, 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

  11. [11]

    H. A. Bethe and G. E. Brown, Evolution of binary compact ob- jects which merge, Astrophys. J.506, 780 (1998), arXiv:astro- ph/9802084

    work page arXiv 1998

  12. [12]

    A Comprehensive Study of Binary Compact Objects as Gravitational Wave Sources: Evolutionary Channels, Rates, and Physical Properties

    K. Belczynski, V . Kalogera, and T. Bulik, A Comprehensive study of binary compact objects as gravitational wave sources: Evolutionary channels, rates, and physical properties, Astro- phys. J.572, 407 (2001), arXiv:astro-ph/0111452

    work page internal anchor Pith review Pith/arXiv arXiv 2001

  13. [13]

    The Formation and Gravitational-Wave Detection of Massive Stellar Black-Hole Binaries

    K. Belczynski, A. Buonanno, M. Cantiello, C. L. Fryer, D. E. Holz, I. Mandel, M. C. Miller, and M. Walczak, The Formation and Gravitational-Wave Detection of Massive Stellar Black-Hole Binaries, Astrophys. J.789, 120 (2014), arXiv:1403.0677 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  14. [14]

    The first gravitational-wave source from the isolated evolution of two 40-100 Msun stars

    K. Belczynski, D. E. Holz, T. Bulik, and R. O’Shaughnessy, The first gravitational-wave source from the isolated evo- lution of two 40-100 Msun stars, Nature534, 512 (2016), arXiv:1602.04531 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  15. [15]

    Formation of the first three gravitational-wave observations through isolated binary evolution

    S. Stevenson, A. Vigna-G ´omez, I. Mandel, J. W. Barrett, C. J. Neijssel, D. Perkins, and S. E. de Mink, Formation of the first three gravitational-wave observations through iso- lated binary evolution, Nature Commun.8, 14906 (2017), arXiv:1704.01352 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  16. [16]

    The progenitors of compact-object binaries: impact of metallicity, common envelope and natal kicks

    N. Giacobbo and M. Mapelli, The progenitors of compact- object binaries: impact of metallicity, common envelope and natal kicks, Mon. Not. Roy. Astron. Soc.480, 2011 (2018), arXiv:1806.00001 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  17. [17]

    Mandel and A

    I. Mandel and A. Farmer, Merging stellar-mass binary black holes, Phys. Rept.955, 1 (2022), arXiv:1806.05820 [astro- ph.HE]

    work page arXiv 2022

  18. [18]

    The Total Merger Rate of Compact Object Binaries In The Local Universe

    A. Sadowski, K. Belczynski, T. Bulik, N. Ivanova, F. A. Ra- sio, and R. W. O’Shaughnessy, The Total Merger Rate of Com- pact Object Binaries In The Local Universe, Astrophys. J.676, 1162 (2008), arXiv:0710.0878 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  19. [19]

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

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  20. [20]

    C. L. Rodriguez, M. Morscher, B. Pattabiraman, S. Chatterjee, C.-J. Haster, and F. A. Rasio, Binary Black Hole Mergers from Globular Clusters: Implications for Advanced LIGO, Phys. Rev. Lett.115, 051101 (2015), [Erratum: Phys.Rev.Lett. 116, 029901 (2016)], arXiv:1505.00792 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  21. [21]

    N. C. Stone, B. D. Metzger, and Z. Haiman, Assisted inspirals of stellar mass black holes embedded in AGN discs: solving the ‘final au problem’, Mon. Not. Roy. Astron. Soc.464, 946 (2017), arXiv:1602.04226 [astro-ph.GA]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  22. [22]

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

    L. Gond ´an, B. Kocsis, P. Raffai, and Z. Frei, Eccentric Black Hole Gravitational-Wave Capture Sources in Galactic Nu- clei: 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

  23. [23]

    Eccentricity distributions of eccentric binary black holes in galactic nuclei

    J. Tak ´atsy, B. B ´ecsy, and P. Raffai, Eccentricity distributions 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

  24. [24]

    Black hole mergers from an evolving population of globular clusters

    G. Fragione and B. Kocsis, Black hole mergers from an evolv- ing population of globular clusters, Phys. Rev. Lett.121, 161103 (2018), arXiv:1806.02351 [astro-ph.GA]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  25. [25]

    Rasskazov and B

    A. Rasskazov and B. Kocsis, The rate of stellar mass black hole scattering in galactic nuclei, Astrophys. J.881, 20 (2019), arXiv:1902.03242 [astro-ph.HE]

    work page arXiv 2019

  26. [26]

    M. A. Sedda, A. W. H. Kamlah, R. Spurzem, F. P. Rizzuto, M. Giersz, T. Naab, and P. Berczik, The dragon-II simulations – III. Compact binary mergers in clusters with up to 1 million stars: mass, spin, eccentricity, merger rate, and pair instabil- ity supernovae rate, Mon. Not. Roy. Astron. Soc.528, 5140 (2024), arXiv:2307.04807 [astro-ph.HE]

    work page arXiv 2024

  27. [27]

    M. K. Singh, B. G. Patterson, and S. Fairhurst, Observability of eccentricity in a population of merging compact binaries, (2025), arXiv:2512.07688 [astro-ph.HE]

    work page arXiv 2025

  28. [28]

    Punturoet al., The Einstein Telescope: A third-generation gravitational wave observatory, Class

    M. Punturoet al., The Einstein Telescope: A third-generation gravitational wave observatory, Class. Quant. Grav.27, 194002 (2010)

    2010

  29. [29]

    TianQin: a space-borne gravitational wave detector

    J. Luoet al.(TianQin), TianQin: a space-borne gravita- tional wave detector, Class. Quant. Grav.33, 035010 (2016), arXiv:1512.02076 [astro-ph.IM]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  30. [30]

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

    D. Reitzeet al., Cosmic Explorer: The U.S. Contribution to 54 Gravitational-Wave Astronomy beyond LIGO, Bull. Am. As- tron. Soc.51, 035 (2019), arXiv:1907.04833 [astro-ph.IM]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  31. [31]

    LISA Definition Study Report

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

    work page internal anchor Pith review Pith/arXiv arXiv 2024

  32. [32]

    von Zeipel, Sur l’application des s ´eries de M

    H. von Zeipel, Sur l’application des s ´eries de M. Lindstedt `a l’´etude du mouvement des com `etes p´eriodiques, Astronomis- che Nachrichten183, 345 (1910)

    1910

  33. [33]

    Kozai, Secular perturbations of asteroids with high incli- nation and eccentricity, The Astronomical Journal67, 591 (1962)

    Y . Kozai, Secular perturbations of asteroids with high incli- nation and eccentricity, The Astronomical Journal67, 591 (1962)

    1962

  34. [34]

    M. L. Lidov, The evolution of orbits of artificial satellites of planets under the action of gravitational perturbations of ex- ternal bodies, Planetary and Space Science9, 719 (1962)

    1962

  35. [35]

    T. O. Kimpson, M. Spera, M. Mapelli, and B. M. Ziosi, Hi- erarchical black hole triples in young star clusters: impact of Kozai–Lidov resonance on mergers, Mon. Not. Roy. Astron. Soc.463, 2443 (2016), arXiv:1608.05422 [astro-ph.GA]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  36. [36]

    J. H. VanLandingham, M. C. Miller, D. P. Hamilton, and D. C. Richardson, The Role of the Kozai–lidov Mechanism in Black Hole Binary Mergers in Galactic Centers, Astrophys. J.828, 77 (2016), arXiv:1604.04948 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  37. [37]

    Black Hole Mergers in Galactic Nuclei Induced by the Eccentric Kozai-Lidov Effect

    B.-M. Hoang, S. Naoz, B. Kocsis, F. A. Rasio, and F. Dosopoulou, Black Hole Mergers in Galactic Nuclei In- duced by the Eccentric Kozai–Lidov Effect, Astrophys. J.856, 140 (2018), arXiv:1706.09896 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  38. [38]

    Fragione, N

    G. Fragione, N. Leigh, and R. Perna, Black hole and neutron star mergers in Galactic Nuclei: the role of triples, Mon. Not. Roy. Astron. Soc.488, 2825 (2019), arXiv:1903.09160 [astro- ph.GA]

    work page arXiv 2019

  39. [39]

    Britt, B

    D. Britt, B. Johanson, L. Wood, M. C. Miller, and E. Michaely, Binary black hole mergers from hierarchical triples in open clusters, Mon. Not. Roy. Astron. Soc.505, 3844 (2021), arXiv:2103.14706 [astro-ph.HE]

    work page arXiv 2021

  40. [40]

    Grishin, I

    E. Grishin, I. M. Romero-Shaw, and A. A. Trani, Gravitational-Wave Signatures of Highly Eccentric Stellar- Mass Binary Black Holes in Galactic Nuclei, (2025), arXiv:2510.13066 [astro-ph.HE]

    work page arXiv 2025

  41. [41]

    S. F. Portegies Zwart and S. McMillan, Black hole mergers in the universe, Astrophys. J. Lett.528, L17 (2000), arXiv:astro- ph/9910061

    work page arXiv 2000

  42. [42]

    M. C. Miller and D. P. Hamilton, Four-body effects in globular cluster black hole coalescence, Astrophys. J.576, 894 (2002), arXiv:astro-ph/0202298

    work page internal anchor Pith review Pith/arXiv arXiv 2002

  43. [43]

    Three-Body Dynamics with Gravitational Wave Emission

    K. Gultekin, M. Coleman Miller, and D. P. Hamilton, Three- body dynamics with gravitational wave emission, Astrophys. J.640, 156 (2006), arXiv:astro-ph/0509885

    work page internal anchor Pith review Pith/arXiv arXiv 2006

  44. [44]

    The Formation of Eccentric Compact Binary Inspirals and the Role of Gravitational Wave Emission in Binary-Single Stellar Encounters

    J. Samsing, M. MacLeod, and E. Ramirez-Ruiz, The For- mation of Eccentric Compact Binary Inspirals and the Role of Gravitational Wave Emission in Binary-Single Stellar En- counters, Astrophys. J.784, 71 (2014), arXiv:1308.2964 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  45. [45]

    On the Assembly Rate of Highly Eccentric Binary Black Hole Mergers

    J. Samsing and E. Ramirez-Ruiz, On the Assembly Rate of Highly Eccentric Binary Black Hole Mergers, Astrophys. J. Lett.840, L14 (2017), arXiv:1703.09703 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  46. [46]

    Eccentric Black Hole Mergers Forming in Globular Clusters

    J. Samsing, Eccentric Black Hole Mergers Forming in Globular Clusters, Phys. Rev. D97, 103014 (2018), arXiv:1711.07452 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  47. [47]

    C. L. Rodriguez, P. Amaro-Seoane, S. Chatterjee, and F. A. Rasio, Post-Newtonian Dynamics in Dense Star Clusters: Highly-Eccentric, Highly-Spinning, and Repeated Binary Black Hole Mergers, Phys. Rev. Lett.120, 151101 (2018), arXiv:1712.04937 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  48. [48]

    Eccentric Black Hole Mergers in Dense Star Clusters: The Role of Binary-Binary Encounters

    M. Zevin, J. Samsing, C. Rodriguez, C.-J. Haster, and E. Ramirez-Ruiz, Eccentric Black Hole Mergers in Dense Star Clusters: The Role of Binary–Binary Encounters, Astrophys. J.871, 91 (2019), arXiv:1810.00901 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  49. [49]

    Arca-Sedda, G

    M. Arca-Sedda, G. Li, and B. Kocsis, Order in the chaos - Eccentric black hole binary mergers in triples formed via strong binary–binary scatterings, Astron. Astrophys.650, A189 (2021), arXiv:1805.06458 [astro-ph.HE]

    work page arXiv 2021

  50. [50]

    Tagawa, B

    H. Tagawa, B. Kocsis, Z. Haiman, I. Bartos, K. Omukai, and J. Samsing, Eccentric Black Hole Mergers in Active Galactic Nuclei, Astrophys. J. Lett.907, L20 (2021), arXiv:2010.10526 [astro-ph.HE]

    work page arXiv 2021

  51. [51]

    Distinguishing Between Formation Channels for Binary Black Holes with LISA

    K. Breivik, C. L. Rodriguez, S. L. Larson, V . Kalogera, and F. A. Rasio, Distinguishing Between Formation Channels for Binary Black Holes with LISA, Astrophys. J. Lett.830, L18 (2016), arXiv:1606.09558 [astro-ph.GA]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  52. [52]

    Constraining stellar binary black hole formation scenarios with eLISA eccentricity measurements

    A. Nishizawa, A. Sesana, E. Berti, and A. Klein, Constrain- ing stellar binary black hole formation scenarios with eLISA eccentricity measurements, Mon. Not. Roy. Astron. Soc.465, 4375 (2017), arXiv:1606.09295 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  53. [53]

    Black Hole Mergers From Globular Clusters Observable by LISA I: Eccentric Sources Originating From Relativistic $N$-body Dynamics

    J. Samsing and D. J. D’Orazio, Black Hole Mergers From Globular Clusters Observable by LISA I: Eccentric Sources Originating From RelativisticN-body Dynamics, Mon. Not. Roy. Astron. Soc.481, 5445 (2018), arXiv:1804.06519 [astro- ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  54. [54]

    Zevin, I

    M. Zevin, I. M. Romero-Shaw, K. Kremer, E. Thrane, and P. D. Lasky, Implications of Eccentric Observations on Binary Black Hole Formation Channels, Astrophys. J. Lett.921, L43 (2021), arXiv:2106.09042 [astro-ph.HE]

    work page arXiv 2021

  55. [55]

    DePorzio, L

    N. DePorzio, L. Randall, and Z.-Z. Xianyu, Mass Beyond Measure: Eccentric Searches for Black Hole Populations, (2024), arXiv:2402.09513 [gr-qc]

    work page arXiv 2024

  56. [56]

    M. A. Sedda, L. Paiella, C. Ugolini, F. Santoliquido, B. Mestichelli, I. Usai, F. Simonato, and M. Branchesi, Iso- lated or Dynamical? Tracing Black Hole Binary Forma- tion through the Population of Gravitational-Wave Sources, (2026), arXiv:2603.20430 [astro-ph.GA]

    work page arXiv 2026

  57. [57]

    D. A. Brown and P. J. Zimmerman, The Effect of Eccentricity on Searches for Gravitational-Waves from Coalescing Com- pact Binaries in Ground-based Detectors, Phys. Rev. D81, 024007 (2010), arXiv:0909.0066 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  58. [58]

    E. A. Huerta and D. A. Brown, Effect of eccentricity on binary neutron star searches in Advanced LIGO, Phys. Rev. D87, 127501 (2013), arXiv:1301.1895 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  59. [59]

    Wang and A

    Y .-F. Wang and A. H. Nitz, Prospects for detecting gravi- tational waves from eccentric subsolar mass compact bina- ries, Astrophys. J.912, 53 (2021), arXiv:2101.12269 [astro- ph.HE]

    work page arXiv 2021

  60. [60]

    Gadre, K

    B. Gadre, K. Soni, S. Tiwari, A. Ramos-Buades, M. Haney, and S. Mitra, Detectability of eccentric binary black holes with matched filtering and unmodeled pipelines during the third observing run of LIGO-Virgo-KAGRA, Phys. Rev. D110, 044013 (2024), arXiv:2405.04186 [gr-qc]

    work page arXiv 2024

  61. [61]

    B. P. Abbottet al.(LIGO Scientific, Virgo), Search for Ec- centric Binary Black Hole Mergers with Advanced LIGO and Advanced Virgo during their First and Second Observ- ing Runs, Astrophys. J.883, 149 (2019), arXiv:1907.09384 [astro-ph.HE]

    work page arXiv 2019

  62. [62]

    A. G. Abacet al.(LIGO Scientific, VIRGO, KAGRA), Search for Eccentric Black Hole Coalescences during the Third Ob- serving Run of LIGO and Virgo, (2023), arXiv:2308.03822 [astro-ph.HE]

    work page arXiv 2023

  63. [63]

    A. H. Nitz, A. Lenon, and D. A. Brown, Search for Eccen- tric Binary Neutron Star Mergers in the first and second ob- serving runs of Advanced LIGO, Astrophys. J.890, 1 (2019), arXiv:1912.05464 [astro-ph.HE]. 55

    work page arXiv 2019

  64. [64]

    A. H. Nitz and Y .-F. Wang, Search for Gravitational Waves from the Coalescence of Subsolar Mass and Eccentric Com- pact Binaries, The Astrophysical Journal915, 54 (2021), arXiv:2102.00868 [astro-ph.HE]

    work page arXiv 2021

  65. [65]

    A. K. Lenon, D. A. Brown, and A. H. Nitz, Eccentric binary neutron star search prospects for Cosmic Explorer, Phys. Rev. D104, 063011 (2021), arXiv:2103.14088 [astro-ph.HE]

    work page arXiv 2021

  66. [66]

    Favata, C

    M. Favata, C. Kim, K. G. Arun, J. Kim, and H. W. Lee, Con- straining the orbital eccentricity of inspiralling compact bi- nary systems with Advanced LIGO, Phys. Rev. D105, 023003 (2022), arXiv:2108.05861 [gr-qc]

    work page arXiv 2022

  67. [67]

    Pal and K

    S. Pal and K. R. Nayak, Swarm-intelligent search for grav- itational waves from eccentric binary mergers, (2023), arXiv:2307.03736 [gr-qc]

    work page arXiv 2023

  68. [68]

    Ravichandran, A

    A. Ravichandran, A. Vijaykumar, S. J. Kapadia, and P. Ku- mar, Rapid Identification and Classification of Eccentric Grav- itational Wave Inspirals with Machine Learning, (2023), arXiv:2302.00666 [gr-qc]

    work page arXiv 2023

  69. [69]

    K. S. Phukon, P. Schmidt, and G. Pratten, A geometric template bank for the detection of spinning low-mass com- pact binaries with moderate orbital eccentricity, (2024), arXiv:2412.06433 [gr-qc]

    work page arXiv 2024

  70. [70]

    Khalouei, C

    E. Khalouei, C. G. Sabiu, H. M. Lee, and A. Gopakumar, External Attention Transformer: A Robust AI Model for Identifying Initial Eccentricity Signatures in Binary Black Hole Events in Simulated Advanced LIGO Data, (2025), arXiv:2506.03634 [gr-qc]

    work page arXiv 2025

  71. [71]

    Wang and A

    Y .-F. Wang and A. H. Nitz, Search for gravitational waves from eccentric binary black holes with an effective-one-body template, (2025), arXiv:2508.05018 [gr-qc]

    work page arXiv 2025

  72. [72]

    Canizares, S

    P. Canizares, S. J. Staelens, and I. Romero-Shaw, The Shape of Eccentricity: Rapid Classification of Eccentric Binaries with the Wavelet Scattering Transform, (2026), arXiv:2602.24079 [gr-qc]

    work page arXiv 2026

  73. [73]

    Systematic parameter errors in inspiraling neutron star binaries

    M. Favata, Systematic parameter errors in inspiraling neu- tron star binaries, Phys. Rev. Lett.112, 101101 (2014), arXiv:1310.8288 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  74. [74]

    Ramos-Buades, S

    A. Ramos-Buades, S. Husa, G. Pratten, H. Estell´es, C. Garc´ıa- Quir´os, M. Mateu-Lucena, M. Colleoni, and R. Jaume, First survey of spinning eccentric black hole mergers: Numerical relativity simulations, hybrid waveforms, and parameter esti- mation, Phys. Rev. D101, 083015 (2020), arXiv:1909.11011 [gr-qc]

    work page arXiv 2020

  75. [75]

    O’Shea and P

    E. O’Shea and P. Kumar, Correlations in gravitational-wave reconstructions from eccentric binaries: A case study with GW151226 and GW170608, Phys. Rev. D108, 104018 (2023), arXiv:2107.07981 [astro-ph.HE]

    work page arXiv 2023

  76. [76]

    Cho, Systematic bias due to eccentricity in parameter estimation for merging binary neutron stars, Phys

    H.-S. Cho, Systematic bias due to eccentricity in parameter estimation for merging binary neutron stars, Phys. Rev. D105, 124022 (2022), arXiv:2205.12531 [gr-qc]

    work page arXiv 2022

  77. [77]

    Gil Choi, T

    H. Gil Choi, T. Yang, and H. M. Lee, Importance of eccen- tricities in parameter estimation of compact binary inspirals with decihertz gravitational-wave detectors, Phys. Rev. D110, 024025 (2024), arXiv:2210.09541 [gr-qc]

    work page arXiv 2024

  78. [78]

    R. Das, V . Gayathri, Divyajyoti, S. Jose, I. Bartos, S. Kli- menko, and C. K. Mishra, Inferring additional physics through unmodelled signal reconstructions, (2024), arXiv:2412.11749 [gr-qc]

    work page arXiv 2024

  79. [79]

    Kumar, S

    Divyajyoti, S. Kumar, S. Tibrewal, I. M. Romero-Shaw, and C. K. Mishra, Blind spots and biases: The dangers of ignoring eccentricity in gravitational-wave signals from binary black holes, Phys. Rev. D109, 043037 (2024), arXiv:2309.16638 [gr-qc]

    work page arXiv 2024

  80. [80]

    Divyajyotiet al., Biased parameter inference of eccentric, spin-precessing binary black holes, (2025), arXiv:2510.04332 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2025

Showing first 80 references.