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arxiv: 2605.15265 · v1 · submitted 2026-05-14 · 🌌 astro-ph.HE · gr-qc

Eccentric Stellar-mass Binary Black Holes: Population, Detectability, and Waveform Analysis in the LISA and LIGO Era

Zeyuan Xuan , Smadar Naoz , Kyle Kremer , Michael L. Katz , Bence Kocsis , Erez Michaely This is my paper

Pith reviewed 2026-05-19 16:13 UTC · model grok-4.3

classification 🌌 astro-ph.HE gr-qc
keywords eccentric binary black holesgravitational wavesLISAdynamical formationMilky Way populationmerger rateswaveform analysis
0
0 comments X p. Extension

The pith

Dynamically formed eccentric stellar-mass black hole binaries produce a detectable population for LISA in the Milky Way and at cosmological distances.

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

The paper builds a catalog of stellar-mass binary black holes formed through dynamical channels including flyby interactions in the Galactic field, eccentric Kozai-Lidov evolution in the Galactic nucleus, and N-body interactions in globular clusters. It predicts that a 10-year LISA observation could detect roughly 36 such highly eccentric sources in the Milky Way at SNR above 1, with the count falling to about 1 at SNR above 50. The same model gives a cosmological merger rate near 9 events per cubic gigaparsec per year and forecasts hundreds of additional extragalactic sources at millihertz frequencies. Eccentric signals can produce independently detectable harmonics that may be mistaken for circular binaries and yield biased chirp-mass estimates. A reader would care because these sources must be included in LISA data analysis to avoid systematic errors in the global fit and to connect formation physics to observable waveforms.

Core claim

The paper claims that a simulated catalog built from the three dominant dynamical formation channels for eccentric stellar-mass BBHs predicts tens of Milky Way detections by LISA at low SNR thresholds, a merger rate of approximately 9 Gpc^{-3} yr^{-1}, hundreds of extragalactic mHz sources at SNR > 1, and distinct eccentricity distributions that affect both detectability and parameter estimation in the LVK band.

What carries the argument

The simulated catalog of dynamically formed eccentric BBHs that incorporates Galactic field flybys, eccentric Kozai-Lidov evolution in the nucleus, and N-body interactions in clusters to generate eccentricity distributions and source counts.

If this is right

  • LISA could detect approximately 36 Milky Way eccentric BBHs with SNR > 1 over a 10-year mission.
  • The model yields a merger rate of roughly 9 Gpc^{-3} yr^{-1}.
  • Hundreds of extragalactic mHz BBHs with SNR > 1 are expected, though the number drops sharply at higher SNR thresholds.
  • Individual harmonics of eccentric signals can be detected separately and may mimic circular binaries with biased chirp masses.
  • Post-Newtonian waveforms converge reliably for these systems at masses up to about 1000 solar masses in the millihertz band.

Where Pith is reading between the lines

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

  • If eccentricity distributions vary measurably between formation channels, LISA data could help determine which channel dominates the observed population.
  • Including eccentric sources in the LISA global fit may reduce systematic biases in parameter recovery for the broader set of gravitational-wave signals.
  • The same catalog approach could be adapted to predict multi-band signals that connect LISA detections to future ground-based observations of the same systems.

Load-bearing premise

The three included dynamical channels fully represent the dominant formation processes for eccentric stellar-mass BBHs without major missing contributions from other mechanisms.

What would settle it

A 10-year LISA dataset that records zero sources with SNR > 1 or a count far outside the predicted range of approximately 36 Milky Way eccentric BBHs would falsify the population estimates.

Figures

Figures reproduced from arXiv: 2605.15265 by Bence Kocsis, Erez Michaely, Kyle Kremer, Michael L. Katz, Smadar Naoz, Zeyuan Xuan.

Figure 1
Figure 1. Figure 1: FIG. 1 [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2 [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3 [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4 [PITH_FULL_IMAGE:figures/full_fig_p009_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5 [PITH_FULL_IMAGE:figures/full_fig_p011_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6 [PITH_FULL_IMAGE:figures/full_fig_p011_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: FIG. 7 [PITH_FULL_IMAGE:figures/full_fig_p012_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: shows a mock realization of dynamically formed BBHs in the Milky Way (which is the same mock popu￾lation as shown in [PITH_FULL_IMAGE:figures/full_fig_p013_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: FIG. 9 [PITH_FULL_IMAGE:figures/full_fig_p014_9.png] view at source ↗
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Figure 10. Figure 10: FIG. 10 [PITH_FULL_IMAGE:figures/full_fig_p014_10.png] view at source ↗
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Figure 11. Figure 11: FIG. 11 [PITH_FULL_IMAGE:figures/full_fig_p015_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: FIG. 12 [PITH_FULL_IMAGE:figures/full_fig_p016_12.png] view at source ↗
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Figure 13. Figure 13: FIG. 13 [PITH_FULL_IMAGE:figures/full_fig_p018_13.png] view at source ↗
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Figure 14. Figure 14: FIG. 14 [PITH_FULL_IMAGE:figures/full_fig_p024_14.png] view at source ↗
read the original abstract

Eccentric binary black holes (BBHs) formed through dynamical interactions can significantly contribute to gravitational wave (GW) detections. In this work, we present a simulated catalog of dynamically-formed, stellar-mass BBHs in the local universe, incorporating contributions from the Galactic field (flyby interactions), Galactic nucleus (eccentric Kozai-Lidov evolution), and globular clusters (N-body interactions). Our results predict a wide, highly eccentric BBH population in the Milky Way (MW), with source counts of $\sim 36, 13, 4.7, 2.3, 1.0$ (for $\mathrm{SNR} > 1, 3, 8, 20, 50$, respectively) during a 10-yr LISA observation. Extending this model to cosmological populations, we show that different dynamical channels can produce distinct eccentricity distributions in the LVK band and can contribute hundreds of additional low-SNR mHz sources. Specifically, our model yields a merger rate of $\Gamma \sim 9 \mathrm{Gpc}^{-3}\mathrm{yr}^{-1}$ and $\sim 490$ extragalactic mHz BBHs with $\mathrm{SNR} > 1$. However, due to the lower mass and weaker GW signals of stellar-mass BBHs, this number declines sharply at higher detection thresholds (e.g., $\sim 1$ for $\mathrm{SNR} > 8$). We further highlight the impact of eccentric BBH signals on the LISA global fit, showing that their individual harmonics can be independently detected in the Milky Way, and may mimic circular binaries with systematically biased chirp masses. Lastly, we show that post-Newtonian waveforms converge reliably for eccentric BBHs with masses of $\lesssim 10^3 M_\odot$ in the mHz band. Overall, eccentric BBHs represent a prevalent and promising target for future space-based GW observatories. The simulated catalog and the LISA Eccentricity Astrophysics Package (LEAP) developed in this work are publicly available at https://github.com/zeyuanxuan/lisa-leap/.

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 constructs a simulated catalog of dynamically formed eccentric stellar-mass BBHs by combining three channels: Galactic-field flyby interactions, nuclear eccentric Kozai-Lidov evolution, and globular-cluster N-body interactions. It reports Milky Way source counts of ∼36, 13, 4.7, 2.3, 1.0 for LISA SNR thresholds >1, 3, 8, 20, 50 over a 10-yr mission, an all-sky merger rate Γ∼9 Gpc^{-3} yr^{-1}, ∼490 extragalactic mHz sources with SNR>1, distinct eccentricity distributions in the LVK band, biases in LISA global-fit chirp-mass recovery, and reliable PN waveform convergence for masses ≲10^3 M_⊙. The catalog and LEAP package are released publicly.

Significance. If the absolute normalizations hold, the work supplies concrete, testable predictions for the eccentric BBH population accessible to LISA and LIGO, quantifies channel-dependent eccentricity signatures, and demonstrates practical impacts on global-fit analyses. The public catalog and software constitute a clear community resource that enables follow-up studies of detectability and parameter biases.

major comments (2)
  1. [Abstract; results on population and detectability] Abstract and results section on MW counts: the headline numbers (∼36 sources for SNR>1, Γ∼9 Gpc^{-3} yr^{-1}) are obtained by summing three forward-modeled channels whose absolute rates rest on assumed densities, binary fractions, and initial conditions. No systematic sensitivity analysis or cross-check against independent eccentric-BBH rate estimates is reported; a factor-of-two shift in any single channel’s normalization (plausible given current uncertainties in GC core densities or nuclear cusp profiles) would rescale the quoted counts by a comparable factor. This directly affects the central claim of specific, observationally relevant source numbers.
  2. [Methods / simulation setup] Section describing the simulation setup and catalog construction: the manuscript states that the catalog “accurately captures the full population” by incorporating the three channels, yet provides neither an error budget on the adopted normalizations nor validation tests (e.g., recovery of known circular BBH rates or comparison with existing dynamical-formation literature). Because the quoted counts and merger rate are outputs of these uncalibrated normalizations rather than direct observables, the robustness of the numerical predictions cannot be assessed from the presented material.
minor comments (2)
  1. [Abstract] The abstract and main text use “∼” for all numerical results; explicit statement of the underlying simulation volume, number of realizations, and statistical uncertainties on the counts would improve clarity.
  2. [Figures on eccentricity and SNR] Figure captions and axis labels for eccentricity distributions and SNR histograms should explicitly note the mass range and frequency band used, to avoid ambiguity when comparing with LVK or LISA sensitivity curves.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive comments and the positive assessment of the manuscript's significance. We address each major comment below, clarifying our approach and outlining revisions to improve the robustness discussion.

read point-by-point responses

  1. Referee: [Abstract; results on population and detectability] Abstract and results section on MW counts: the headline numbers (∼36 sources for SNR>1, Γ∼9 Gpc^{-3} yr^{-1}) are obtained by summing three forward-modeled channels whose absolute rates rest on assumed densities, binary fractions, and initial conditions. No systematic sensitivity analysis or cross-check against independent eccentric-BBH rate estimates is reported; a factor-of-two shift in any single channel’s normalization (plausible given current uncertainties in GC core densities or nuclear cusp profiles) would rescale the quoted counts by a comparable factor. This directly affects the central claim of specific, observationally relevant source numbers.

    Authors: We agree that the quoted source counts and merger rate depend on literature-based normalizations for densities, binary fractions, and initial conditions, which carry uncertainties. The manuscript presents results for a fiducial model combining the three channels, with emphasis on relative channel contributions and eccentricity signatures rather than absolute precision. In revision, we will add a sensitivity analysis subsection varying the dominant normalization parameters (e.g., globular cluster core density and nuclear cusp profile) by factors of 0.5 and 2, reporting the resulting ranges for Milky Way counts and the merger rate. We will also expand the discussion to compare our fiducial merger rate against independent dynamical BBH formation estimates in the literature. The public release of the catalog and LEAP code already enables community exploration of alternative normalizations. revision: yes

  2. Referee: [Methods / simulation setup] Section describing the simulation setup and catalog construction: the manuscript states that the catalog “accurately captures the full population” by incorporating the three channels, yet provides neither an error budget on the adopted normalizations nor validation tests (e.g., recovery of known circular BBH rates or comparison with existing dynamical-formation literature). Because the quoted counts and merger rate are outputs of these uncalibrated normalizations rather than direct observables, the robustness of the numerical predictions cannot be assessed from the presented material.

    Authors: The phrasing 'accurately captures the full population' was meant to convey inclusion of the principal dynamical channels rather than exact normalizations. We will revise this language in the methods section for precision. We will add an explicit error budget paragraph summarizing uncertainties in the adopted literature values. For validation, we will include a comparison of the total merger rate (in the circular limit) to published dynamical formation rates from other works. These changes will be incorporated into the revised methods and results sections to allow readers to evaluate robustness directly. revision: yes

Circularity Check

0 steps flagged

No significant circularity; predictions are forward-model outputs from assumed channel normalizations

full rationale

The quoted source counts (~36 for SNR>1 in MW) and merger rate (Γ∼9 Gpc^{-3} yr^{-1}) are generated by running a multi-channel simulation that sums contributions from Galactic-field flybys, nuclear KL evolution, and globular-cluster N-body interactions. These numbers follow directly from the chosen densities, binary fractions, and initial conditions fed into the catalog; they are not defined in terms of the target counts themselves, nor do any equations reduce the output to a fit of the same quantities. No self-citation chain is shown to be load-bearing for the absolute normalization, and the paper does not rename a known result or smuggle an ansatz via prior work. The derivation remains self-contained against external benchmarks even if the input normalizations carry astrophysical uncertainty.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The central claims rest on the accuracy of the three-channel dynamical formation model, the post-Newtonian waveform approximations for eccentric systems, and the scaling from Milky Way to cosmological volumes.

free parameters (1)
  • simulation parameters for interaction rates and initial conditions
    The population synthesis and N-body models require numerous parameters for stellar densities, velocity dispersions, and binary fractions that are set from astrophysical priors or prior simulations.
axioms (1)
  • domain assumption Dynamical interactions in the Galactic field, nucleus, and globular clusters are the primary channels producing the eccentric stellar-mass BBH population modeled here
    The catalog is constructed by adding contributions from these three specific channels as described in the abstract.

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Reference graph

Works this paper leans on

121 extracted references · 121 canonical work pages · 40 internal anchors

  1. [1]

    Abbott, R

    B. Abbott, R. Abbott, T. Abbott,et al., Physi- cal Review Letters116, 10.1103/physrevlett.116.061102 (2016)

    work page doi:10.1103/physrevlett.116.061102 2016

  2. [2]

    The LIGO Scientific Collaboration, the Virgo Col- laboration, the KAGRA Collaboration,et al., arXiv e-prints , arXiv:2111.03634 (2021), arXiv:2111.03634 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2021

  3. [3]

    Abbott, T

    R. Abbott, T. D. Abbott, F. Acernese,et al.(LIGO Scientific Collaboration, Virgo Collaboration, and KA- GRA Collaboration), Phys. Rev. X13, 041039 (2023)

    work page 2023

  4. [4]

    Amaro-Seoane, J

    P. Amaro-Seoane, J. Andrews, M. Arca Sedda,et al., Living Reviews in Relativity26, 10.1007/s41114-022- 00041-y (2023)

    work page doi:10.1007/s41114-022- 2023

  5. [5]

    TianQin: a space-borne gravitational wave detector

    J. Luo, L.-S. Chen, H.-Z. Duan, Y.-G. Gong, S. Hu, J. Ji, Q. Liu, J. Mei, V. Milyukov, M. Sazhin, C.-G. Shao, V. T. Toth, H.-B. Tu, Y. Wang, Y. Wang, H.- C. Yeh, M.-S. Zhan, Y. Zhang, V. Zharov, and Z.-B. Zhou, CQG33, 035010 (2016), arXiv:1512.02076 [astro- ph.IM]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  6. [6]

    W.-H. Ruan, C. Liu, Z.-K. Guo, Y.-L. Wu, and R.-G. Cai, Nature Astronomy4, 108 (2020)

    work page 2020

  7. [7]

    P. C. Peters, Physical Review136, 1224 (1964)

    work page 1964

  8. [8]

    LISA Capture Sources: Approximate Waveforms, Signal-to-Noise Ratios, and Parameter Estimation Accuracy

    L. Barack and C. Cutler, Phys. Rev. D69, 082005 (2004), gr-qc/0310125

    work page internal anchor Pith review Pith/arXiv arXiv 2004

  9. [9]

    Parameter estimation for inspiraling eccentric compact binaries including pericenter precession

    B. Mik´ oczi, B. Kocsis, P. Forg´ acs, and M. Vas´ uth, Phys. Rev. D86, 104027 (2012), arXiv:1206.5786 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  10. [10]

    Detecting hierarchical stellar systems with LISA

    T. Robson, N. J. Cornish, N. Tamanini, and S. Toonen, Phys. Rev. D98, 064012 (2018), arXiv:1806.00500 [gr- qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  11. [11]

    Chen, Z.-Y

    X. Chen, Z.-Y. Xuan, and P. Peng, Astrophys. J.896, 171 (2020), arXiv:2003.08639 [astro-ph.HE]

    work page arXiv 2020

  12. [12]

    Amaro-Seoaneet al., arXiv e-prints , arXiv:2203.06016 (2022), arXiv:2203.06016 [gr-qc]

    P. Amaro-Seoaneet al., arXiv e-prints , arXiv:2203.06016 (2022), arXiv:2203.06016 [gr-qc]

    work page arXiv 2022

  13. [13]

    Detecting Supermassive Black Hole-Induced Binary Eccentricity Oscillations with LISA

    B.-M. Hoang, S. Naoz, B. Kocsis, W. M. Farr, and J. McIver, Astrophys. J. Lett.875, L31 (2019), arXiv:1903.00134 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  14. [14]

    Y. Fang, X. Chen, and Q.-G. Huang, Astrophys. J.887, 210 (2019), arXiv:1908.01443 [astro-ph.HE]. 20

    work page arXiv 2019

  15. [15]

    Tamanini, A

    N. Tamanini, A. Klein, C. Bonvin, E. Barausse, and C. Caprini, Phys. Rev. D101, 063002 (2020), arXiv:1907.02018 [astro-ph.IM]

    work page arXiv 2020

  16. [16]

    Torres-Orjuela, P

    A. Torres-Orjuela, P. Amaro Seoane, Z. Xuan, A. J. K. Chua, M. J. B. Rosell, and X. Chen, Phys. Rev. Lett. 127, 041102 (2021), arXiv:2010.15842 [gr-qc]

    work page arXiv 2021

  17. [17]

    Z. Xuan, P. Peng, and X. Chen, Mon. Not. R. Astron. Soc.502, 4199 (2021), arXiv:2012.00049 [astro-ph.HE]

    work page arXiv 2021

  18. [18]

    Z. Xuan, S. Naoz, and X. Chen, Phys. Rev. D107, 043009 (2023), arXiv:2210.03129 [astro-ph.HE]

    work page arXiv 2023

  19. [19]

    Z. Xuan, S. Naoz, A. K. Y. Li, B. Kocsis, E. Pe- tigura, A. M. Knee, J. McIver, K. Kremer, and W. M. Farr, arXiv e-prints , arXiv:2409.15413 (2024), arXiv:2409.15413 [astro-ph.HE]

    work page arXiv 2024

  20. [20]

    Z. Xuan, C. Shariat, and S. Naoz, From wide triples to ucxbs: Multimessenger signatures of dynamically- formed black hole-white dwarf systems in the lisa band (2025), arXiv:2508.13264 [astro-ph.HE]

    work page arXiv 2025

  21. [21]

    The promise of multi-band gravitational wave astronomy

    A. Sesana, Physical Review Letters116, 231102 (2016), arXiv:1602.06951 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  22. [22]

    X. Fang, T. A. Thompson, and C. M. Hirata, The As- trophysical Journal875, 75 (2019)

    work page 2019

  23. [23]

    T. L. S. Collaboration, the Virgo Collaboration, the KAGRA Collaboration,et al., Gwtc-4.0: An introduc- tion to version 4.0 of the gravitational-wave transient catalog (2025), arXiv:2508.18080 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  24. [24]

    B. P. Abbott, R. Abbott, T. D. Abbott,et al., Astro- phys. J.883, 149 (2019)

    work page 2019

  25. [25]

    A. K. Lenon, A. H. Nitz, and D. A. Brown, Monthly Notices of the Royal Astronomical Society497, 1966 (2020)

    work page 1966

  26. [26]

    Romero-Shaw, P

    I. Romero-Shaw, P. D. Lasky, E. Thrane, and J. C. Bustillo, The Astrophysical Journal Letters903, L5 (2020)

    work page 2020

  27. [27]

    Zevin, I

    M. Zevin, I. M. Romero-Shaw, K. Kremer, E. Thrane, and P. D. Lasky, The Astrophysical Journal Letters921, L43 (2021)

    work page 2021

  28. [28]

    Gayathri, J

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

    work page arXiv 2022

  29. [29]

    R. M. O’Leary, B. Kocsis, and A. Loeb, Mon. Not. R. Astron. Soc.395, 2127 (2009), arXiv:0807.2638 [astro- ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  30. [30]

    Kocsis and J

    B. Kocsis and J. Levin, Physical Review D85, 10.1103/physrevd.85.123005 (2012)

    work page doi:10.1103/physrevd.85.123005 2012

  31. [31]

    Distinguishing Between Formation Channels for Binary Black Holes with LISA

    K. Breivik, C. L. Rodriguez, S. L. Larson, V. Kalogera, and F. A. Rasio, Astrophys. J. Lett.830, L18 (2016), arXiv:1606.09558

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  32. [32]

    C. L. Rodriguez, S. Chatterjee, and F. A. Rasio, Phys. Rev. D93, 084029 (2016), arXiv:1602.02444 [astro- ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  33. [33]

    D. J. D’Orazio and J. Samsing, Mon. Not. R. Astron. Soc.481, 4775 (2018), arXiv:1805.06194 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  34. [34]

    Post-Newtonian Dynamics in Dense Star Clusters: Binary Black Holes in the LISA Band

    K. Kremer, C. L. Rodriguez, P. Amaro-Seoane, K. Breivik, S. Chatterjee, M. L. Katz, S. L. Larson, F. A. Rasio, J. Samsing, C. S. Ye, and M. Zevin, Phys. Rev. D99, 063003 (2019), arXiv:1811.11812 [astro- ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  35. [35]

    Zevin, J

    M. Zevin, J. Samsing, C. Rodriguez, C.-J. Haster, and E. Ramirez-Ruiz, The Astrophysical Journal871, 91 (2019)

    work page 2019

  36. [36]

    Samsing, A

    J. Samsing, A. S. Hamers, and J. G. Tyles, Phys. Rev. D100, 043010 (2019), arXiv:1906.07189 [astro-ph.HE]

    work page arXiv 2019

  37. [37]

    M. A. S. Martinez, G. Fragione, K. Kremer, S. Chatter- jee, C. L. Rodriguez, J. Samsing, C. S. Ye, N. C. Weath- erford, M. Zevin, S. Naoz, and F. A. Rasio, Astrophys. J.903, 67 (2020), arXiv:2009.08468 [astro-ph.GA]

    work page arXiv 2020

  38. [38]

    Antonini and M

    F. Antonini and M. Gieles, Mon. Not. R. Astron. Soc. 492, 2936 (2020), arXiv:1906.11855 [astro-ph.HE]

    work page arXiv 2020

  39. [39]

    Winter-Grani´ c, C

    M. Winter-Grani´ c, C. Petrovich, and V. Pe˜ na-Donaire, Binary mergers in the centers of galaxies: syn- ergy between stellar flybys and tidal fields (2023), arXiv:2312.17319 [astro-ph.GA]

    work page arXiv 2023

  40. [40]

    Z. Xuan, K. Kremer, and S. Naoz, The Astrophysical Journal Letters985, L42 (2025)

    work page 2025

  41. [41]

    Kozai, Astron

    Y. Kozai, Astron. J.67, 591 (1962)

    work page 1962

  42. [42]

    M. L. Lidov, Planetary and Space Sci.9, 719 (1962)

    work page 1962

  43. [43]

    The Eccentric Kozai-Lidov Effect and Its Applications

    S. Naoz, Annu. Rev. Astron. Astrophys.54, 441 (2016), arXiv:1601.07175 [astro-ph.EP]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  44. [44]

    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, Astrophys. J.856, 140 (2018), arXiv:1706.09896 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  45. [45]

    A. P. Stephan, S. Naoz, A. M. Ghez, M. R. Morris, A. Ciurlo, T. Do, K. Breivik, S. Coughlin, and C. L. Ro- driguez, Astrophys. J.878, 58 (2019), arXiv:1903.00010 [astro-ph.SR]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  46. [46]

    Observing Eccentricity Oscillations of Binary Black Holes in LISA

    L. Randall and Z.-Z. Xianyu, arXiv e-prints , arXiv:1902.08604 (2019), arXiv:1902.08604 [astro- ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 1902

  47. [47]

    M. W. Bub and C. Petrovich, Astrophys. J.894, 15 (2020), arXiv:1910.02079 [astro-ph.HE]

    work page arXiv 2020

  48. [48]

    Deme, B.-M

    B. Deme, B.-M. Hoang, S. Naoz, and B. Kocsis, The Astrophysical Journal901, 125 (2020)

    work page 2020

  49. [49]

    H. Wang, A. P. Stephan, S. Naoz, B.-M. Hoang, and K. Breivik, Astrophys. J.917, 76 (2021), arXiv:2010.15841 [astro-ph.HE]

    work page arXiv 2021

  50. [50]

    Z. Xuan, S. Naoz, B. Kocsis, and E. Michaely, arXiv e-prints , arXiv:2310.00042 (2023), arXiv:2310.00042 [astro-ph.HE]

    work page arXiv 2023

  51. [51]

    A. M. Knee, J. McIver, S. Naoz, I. M. Romero-Shaw, and B.-M. Hoang, Detecting gravitational-wave bursts from black hole binaries in the galactic center with lisa (2024), arXiv:2404.12571 [astro-ph.HE]

    work page arXiv 2024

  52. [52]

    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 (2026), arXiv:2510.13066 [astro-ph.HE]

    work page arXiv 2026

  53. [53]

    Detection Rate Estimates of Gravity-waves Emitted During Parabolic Encounters of Stellar Black Holes in Globular Clusters

    B. Kocsis, M. E. G´ asp´ ar, and S. M´ arka, Astrophys. J. 648, 411 (2006), astro-ph/0603441

    work page internal anchor Pith review Pith/arXiv arXiv 2006

  54. [54]

    Michaely and H

    E. Michaely and H. B. Perets, Astrophys. J. Lett.887, L36 (2019), arXiv:1902.01864 [astro-ph.SR]

    work page arXiv 2019

  55. [55]

    Michaely and H

    E. Michaely and H. B. Perets, Mon. Not. R. Astron. Soc. 498, 4924 (2020), arXiv:2008.01094 [astro-ph.HE]

    work page arXiv 2020

  56. [56]

    Michaely and S

    E. Michaely and S. Naoz, Astrophys. J.936, 184 (2022), arXiv:2205.15040 [astro-ph.HE]

    work page arXiv 2022

  57. [57]

    Stegmann, A

    J. Stegmann, A. Vigna-G´ omez, A. Rantala, T. Wagg, L. Zwick, M. Renzo, L. A. C. van Son, S. E. de Mink, and S. D. M. White, The Astrophysical Journal Letters 972, L19 (2024)

    work page 2024

  58. [58]

    Tagawa, B

    H. Tagawa, B. Kocsis, Z. Haiman, I. Bartos, K. Omukai, and J. Samsing, Astrophys. J. Lett.907, L20 (2021), arXiv:2010.10526 [astro-ph.HE]

    work page arXiv 2021

  59. [59]

    Peng and X

    P. Peng and X. Chen, Mon. Not. R. Astron. Soc.505, 1324 (2021), arXiv:2104.07685 [astro-ph.HE]. 21

    work page arXiv 2021

  60. [60]

    Samsing, I

    J. Samsing, I. Bartos, D. J. D’Orazio, Z. Haiman, B. Kocsis, N. W. C. Leigh, B. Liu, M. E. Pessah, and H. Tagawa, Nature603, 237 (2022), arXiv:2010.09765 [astro-ph.HE]

    work page arXiv 2022

  61. [61]

    D. J. Mu˜ noz, N. C. Stone, C. Petrovich, and F. A. Rasio, arXiv e-prints , arXiv:2204.06002 (2022), arXiv:2204.06002 [astro-ph.HE]

    work page arXiv 2022

  62. [62]

    Gautham Bhaskar, G

    H. Gautham Bhaskar, G. Li, and D. Lin, arXiv e-prints , arXiv:2303.12539 (2023), arXiv:2303.12539 [astro- ph.HE]

    work page arXiv 2023

  63. [63]

    K. S. Tai, S. T. McWilliams, and F. Pretorius, Physical Review D90, 10.1103/physrevd.90.103001 (2014)

    work page doi:10.1103/physrevd.90.103001 2014

  64. [64]

    Loutrel and N

    N. Loutrel and N. Yunes, Classical and Quantum Grav- ity34, 135011 (2017)

    work page 2017

  65. [65]

    Loutrel, arXiv e-prints , arXiv:2009.11332 (2020), arXiv:2009.11332 [gr-qc]

    N. Loutrel, arXiv e-prints , arXiv:2009.11332 (2020), arXiv:2009.11332 [gr-qc]

    work page arXiv 2009

  66. [66]

    Romero-Shaw, N

    I. Romero-Shaw, N. Loutrel, and M. Zevin, Phys. Rev. D107, 122001 (2023), arXiv:2211.07278 [gr-qc]

    work page arXiv 2023

  67. [67]

    Z. Xuan, S. Naoz, B. Kocsis, and E. Michaely, Phys. Rev. D110, 023020 (2024)

    work page 2024

  68. [68]

    T. A. Thompson, Astrophys. J.741, 82 (2011), arXiv:1011.4322 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  69. [69]

    Hoang, S

    B.-M. Hoang, S. Naoz, and K. Kremer, Astrophys. J. 903, 8 (2020), arXiv:2007.08531 [astro-ph.HE]

    work page arXiv 2020

  70. [70]

    S. Naoz, C. M. Will, E. Ramirez-Ruiz, A. Hees, A. M. Ghez, and T. Do, Astrophys. J. Lett.888, L8 (2020), arXiv:1912.04910 [astro-ph.GA]

    work page arXiv 2020

  71. [71]

    P. C. Peters and J. Mathews, Physical Review131, 435 (1963)

    work page 1963

  72. [72]

    Science with the space-based interferometer eLISA. I: Supermassive black hole binaries

    A. Klein, E. Barausse, A. Sesana, A. Petiteau, E. Berti, S. Babak, J. Gair, S. Aoudia, I. Hinder, F. Ohme, and B. Wardell, Phys. Rev. D93, 024003 (2016), arXiv:1511.05581 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  73. [73]

    The construction and use of LISA sensitivity curves

    T. Robson, N. J. Cornish, and C. Liu, Classical and Quantum Gravity36, 105011 (2019), arXiv:1803.01944 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  74. [74]

    Emami and A

    R. Emami and A. Loeb, Mon. Not. R. Astron. Soc.495, 536 (2020), arXiv:1910.04828 [astro-ph.GA]

    work page arXiv 2020

  75. [75]

    Naoz and Z

    S. Naoz and Z. Haiman, arXiv e-prints , arXiv:2307.11149 (2023), arXiv:2307.11149 [astro- ph.HE]

    work page arXiv 2023

  76. [76]

    L. S. Finn and K. S. Thorne, Physical Review D62, 10.1103/physrevd.62.124021 (2000)

    work page doi:10.1103/physrevd.62.124021 2000

  77. [77]

    C. J. Moore, R. H. Cole, and C. P. L. Berry, Classical and Quantum Gravity32, 015014 (2014)

    work page 2014

  78. [78]

    Kupfer, V

    T. Kupfer, V. Korol, S. Shah, G. Nelemans, T. R. Marsh, G. Ramsay, P. J. Groot, D. T. H. Steeghs, and E. M. Rossi, Monthly Notices of the Royal Astronomical Society480, 302 (2018)

    work page 2018

  79. [79]

    T. M. Tauris, Physical Review Letters121, 10.1103/physrevlett.121.131105 (2018)

    work page doi:10.1103/physrevlett.121.131105 2018

  80. [80]

    L. S. Collaboration and V. Collaboration (LIGO Scien- tific Collaboration and Virgo Collaboration), Phys. Rev. Lett.125, 101102 (2020)

    work page 2020

Showing first 80 references.