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REVIEW 3 major objections 6 minor 43 references

Coincident morphological transitions in precessing black-hole binaries

T0 review · 3 major / 6 minor · reviewed 2026-08-05 · deepseek-v4-flash

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Pith's one-line read Every double and triple spin-morphology transition in inspiraling black-hole binaries is now mapped in closed form: five of six double cases admit precessing solutions, the down-up pair is forbidden, and two triple configurations exist.

desk verdict Solid extension completing the analytic taxonomy of coincident spin-morphology transitions, with a real completeness caveat in footnote 3 and some compressed algebra. read the letter →

arxiv 2508.19735 v1 pith:EZR4HNPA submitted 2025-08-27 gr-qc astro-ph.HE

Davide Gerosa , Giulia Foroni , Giulia Fumagalli , Emanuele Berti This is my paper
classification gr-qcastro-ph.HE PACS 04.25.Nx04.30.-w
keywords black-holebinariesspinprecessionpost-Newtonianapproximationmorphologiesmorphologicaltransitionsmulti-timescaledynamicsup-downinstabilitygravitational-waveastronomy
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

Black-hole binaries with misaligned spins precess, and as gravitational-wave emission shrinks the orbit, the character of that precession can change class — switching between circulating and librating spin morphologies. This paper asks when two or three of those morphological transitions can occur within the same precession cycle rather than sequentially, and shows that every such coincident case is analytically closed-form. Requiring the conserved effective spin and the asymptotic angular momentum to take the same values at both turning points of the precession cycle yields six pairwise conditions: five admit precessing solutions with explicit formulas, one (the down-up configuration) is forbidden, and exactly two triple-transition binaries exist. A single closed-form orbital separation, rwide, governs where the rare C− morphology becomes accessible, and it analytically explains the earlier empirical finding that multiple transitions prefer nearly equal masses with unequal spin magnitudes. These fully precessing systems transiently align both spins with the orbital angular momentum, making them concrete targets for gravitational-wave searches.

What carries the argument

The load-bearing object is the multi-timescale parametrization of spin precession: the conserved effective spin χeff, the asymptotic angular momentum κ (constant on the precession timescale, secularly driven by radiation reaction), and the weighted spin difference δχ, which oscillates between endpoints δχ± and encodes the precession cycle. The monotonicity relations d cosθ1/dδχ ≥ 0 and d cosθ2/dδχ ≤ 0 reduce the eight naively possible alignment events to four viable transition conditions, and the requirement that χeff and κ take identical values at both endpoints gives the two algebraic equations (3.1)–(3.2) that every coincident-transition solution must satisfy. Solving these for the six pa

What would settle it

Integrate an ensemble of binaries with isotropic spin directions at r = 10⁶M down to r = 10M using the full orbit-averaged (not precession-averaged) spin equations, and measure the first separation at which any binary enters the C− morphology for fixed (q, χ1, χ2): if the onset does not coincide with rwide = ((χ1 − qχ2)/(1 − q))²M, the central prediction fails. A sharper version: take the triple-transition parameters of Eqs. (3.10)–(3.11), evolve the exact 2PN equations through one precession cycle, and verify that all three alignment conditions (for example cos θ1− = −1, cos θ1+ = +1, cos θ2+

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Extended reading notes

Core claim

From the four viable alignment conditions (cos θ1− = −1, cos θ1+ = +1, cos θ2− = +1, cos θ2+ = −1), this paper constructs the six possible concurrent pairs of morphological transitions and solves each analytically by requiring that the conserved effective spin χeff and the asymptotic angular momentum κ take the same values at both endpoints δχ± of a precession cycle. Cases 1–2 are wide nutation of one hole (allowed only at r ≤ rwide); cases 3–4 are one-parameter families with both holes aligning at r = rwide, the morphology jumping directly from C+ to C−; case 5 recovers the up-down instability band rUD− ≤ r ≤ rUD+; case 6, down-up, admits only the non-precessing solution. Intersecting the s

Load-bearing premise

The whole taxonomy rests on the timescale hierarchy t_orb ≪ t_pre ≪ t_rad, which justifies averaging over orbits and precession cycles and treating the inspiral as quasi-adiabatic; near merger, where radiation reaction becomes competitive with precession, the analytic coincident-transition conditions are not expected to hold.

Editorial extensions

If this is right

  • The separation rwide from Eq. (3.4) is exactly where the C− morphology becomes accessible during inspiral, turning an earlier heuristic observation about multiple transitions into an analytic prediction based only on (q, χ1, χ2).
  • The coincident double transitions of cases 1–4 take the binary directly from C+ to C− within one precession cycle, with no intermediate librating phase; the up-down case 5 instead produces standard C+ → L0 or Lπ → C− transitions at a single endpoint.
  • The up-down configuration is unstable precisely on rUD− ≤ r ≤ rUD+, a result the coincident-condition calculation re-derives, while the mirror down-up configuration is stable at all separations.
  • Exactly two fine-tuned binaries in the whole parameter space undergo triple transitions, each requiring r = rwide and a fixed value of the effective spin χeff = (χ1 − qχ2)/(1 + q).
  • The analytic conditions give gravitational-wave searches concrete target parameters: binaries inferred to occupy the C− morphology are indirect evidence of the double-transition mechanism, and the λ families of Eqs. (3.6)–(3.7) enumerate the configurations that cross it.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • Because χeff takes the same fixed value (χ1 − qχ2)/(1 + q) at both triple-transition points and at the up-down band center, the effective spin — not the individual tilt angles — is likely the sharpest search variable for locating these events in gravitational-wave catalogs.
  • A testable extension: evolve full ensembles through the exact rwide crossing with precession-averaged equations and record the spread in the C− onset separation produced by finite precession-cycle averaging; the width of that spread quantifies how cleanly the predicted onset survives.
  • If the taxonomy holds up under full numerical relativity, binaries found near the λ families of Eqs. (3.6)–(3.7) would be clear candidates for double-alignment events — two transient full alignments in one precession cycle — which waveform models built on single-transition morphology changes may not represent.
  • The paper's restriction to quasi-circular orbits suggests an immediate open direction: the same coincident-condition construction applied to eccentric or neutron-star binaries could reveal whether the rwide scale persists or acquires eccentricity corrections.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 6 minor

Summary. The paper studies post-Newtonian spin precession in black-hole binaries using the multi-timescale framework. It claims to systematically map all cases of coincident morphological transitions—instances in which two or three morphological transitions occur within the same precession cycle. From four viable transition conditions (cos θ1− = −1, cos θ1+ = +1, cos θ2− = +1, cos θ2+ = −1), the authors enumerate six pairwise combinations, provide analytic solutions for five of them and identify one as forbidden, and further identify two triple-transition configurations. A key derived quantity is rwide, the separation at which the C− morphology becomes accessible. The results are checked against numerical integrations using the public precession module. The central claim is that all coincident transitions can be characterized analytically.

Significance. If the completeness claim is correct, this is a valuable closed-form taxonomy of an intricate phenomenon in PN spin precession. The paper gives an analytic foundation for previously empirical observations about when C− morphologies appear, and it connects wide nutation and up-down instabilities to the general framework of coincident transitions. A notable strength is that the analytic radii and conditions are derived from constants of motion rather than fitted; the family label λ is a parameter of the solution family, not a fit to data. The numerical confirmation uses an independent public implementation of the same PN equations, so it is non-circular. However, the central completeness claim is weakened by an admitted unresolved case, and the derivation of the analytic solutions is not shown in the manuscript.

major comments (3)
  1. [§3.1, footnote 3] The abstract and Section 3 state that all coincident morphological transitions can be mapped and characterized analytically. Footnote 3 however admits: "two transitions occurring at δχ− and δχ+ could also result in the spin morphology evolving between the two librating classes without an intermediate phase of circulation. While we were not able to exclude this possibility analytically, we could not identify any of these cases even after extensive numerical investigations." This is a direct and acknowledged exception to the completeness claim. The six pairwise combinations listed in Section 3 are only the viable endpoint conditions; if an L0↔Lπ direct transition exists, it is either one of these branches with a different morphological outcome or an unrecognized mechanism. Either way, "all such cases" is not proven. The numerical runs in Fig. 2 all start from C+ at large separation, so the
  2. [§3, Eqs. (3.3)–(3.11)] The analytic solutions for the six cases and the two triple transitions are stated after inserting the endpoint conditions into Eqs. (3.1) and (3.2), but the actual algebra is not shown. The text does not demonstrate how the "only if" conditions are derived, how trivial vs. non-trivial solutions are separated, or why no other solutions exist for a given case. For a paper whose contribution is a systematic and complete taxonomy, the absence of this derivation makes it impossible for the reader to verify exhaustiveness. This is especially important because the completeness claim in the abstract relies on these solutions being the only ones. At minimum, the derivation should be included in an appendix or a supplementary file, with each step leading from Eqs. (3.1)–(3.2) to the corresponding solution family.
  3. [§3.7] The claim that "there are only two" triple-transition configurations is asserted without proof. The paper states this follows straightforwardly from the preceding conditions, but since the preceding solutions themselves are not derived, the uniqueness of Eqs. (3.10) and (3.11) is not established. The numerical examples in Fig. 2 only illustrate the two claimed cases; they do not rule out other triple combinations. This should be addressed together with the missing derivation of the pairwise cases.
minor comments (6)
  1. [Fig. 1 caption] The caption lists "χ1 = 0.5, χ1 = 1" but the second should be χ2 = 1.
  2. [§3.2] Text reads "χeff ≃= 0.36" with a double equals sign; should be χeff ≃ 0.36 or = 0.36.
  3. [§3.5] The inequality "rUD− ≤ rwide < rUD−" should presumably read "rUD− ≤ rwide < rUD+".
  4. [§3.4] In the text, "the conditions cos θ1− = +1, cos θ2+ = +1 are satisfied when..." is inconsistent with case 4 of the enumeration, which is cos θ1+ = +1, cos θ2− = +1. Please correct the sign/placement of the plus conditions.
  5. [§3.7] In the examples, "χ1 = 0.3, and χ1 = 0.8" should be χ2 = 0.8, and "χ1 = 0.8, and χ1 = 0.5" should be χ2 = 0.5.
  6. [§3.5] Typo: "trasition" should be "transition".

Circularity Check

0 steps flagged · score 1.0 of 10

No significant circularity: coincident-transition conditions are solved from the constants of motion; footnote 3 admits a non-circular completeness gap.

full rationale

The paper's derivations are self-contained: Eqs. (3.1)-(3.2) enforce equality of the constants of motion χeff and κ at the two precession endpoints, a necessary condition that does not fit any parameter to the predicted transitions. The closed-form radii and conditions (3.3)-(3.11) are algebraic consequences of the 2PN precession equations and the 1PN radiation-reaction equations. The numerical checks use the public precession module, an independent implementation of the same equations, so they provide genuine confirmation rather than circular support. Self-citations ([12,14,18,22,26]) supply the morphology classification, the four viable transition conditions, and prior results such as wide nutation and the up-down instability; these are prior analytic results with stated assumptions, and the paper's new contribution is the systematic enumeration and solution of the six pairwise cases. Footnote 3 (Sec. 3.1) explicitly acknowledges an unresolved possibility of a direct L0↔Lπ double transition, stating 'we were not able to exclude this possibility analytically' nor find it numerically; this is a completeness limitation, not a circular reduction, and it does not make the derived conditions equivalent to their inputs. The free parameter λ in cases 3 and 4 is a family label, not a fitted value. Overall, the central claim is derived, not assumed, and the score reflects only the heavy reliance on the authors' prior framework.

Assumptions & free parameters 1 free parameters · 4 assumptions · 0 invented entities

No new physical entities are introduced. The only free parameter is the family label lambda; all binary parameters (q, chi1, chi2, chi_eff, kappa, r) come from the standard PN description. The axioms are the standard timescale separation, the PN truncation, the constancy of chi_eff and kappa, and the monotonicity inequalities that restrict alignment conditions to four.

free parameters (1)
  • lambda = -1 <= lambda <= 1
    Labels a one-parameter family of solutions in cases 3 and 4 (Eqs. 3.6 and 3.7). For fixed q, chi1, chi2 and a chosen lambda, the binary must have specific chi_eff and kappa. It is not fitted to data; it is a continuous degeneracy of the solution family.
assumptions (4)
  • domain assumption Timescale hierarchy t_orb << t_pre << t_rad allowing precession-averaged quasi-adiabatic evolution
    Stated in Section 2; the entire morphological classification and the secular ODE for kappa depend on this separation.
  • domain assumption 2PN spin-precession and 1PN precession-averaged radiation-reaction equations are the correct effective dynamics
    Used throughout; the paper takes the PN equations from Refs. [27] and [26] without testing the truncation except for the up-down case versus NR in Ref. [37].
  • domain assumption Only four alignment conditions are viable, as implied by the monotonicity inequalities in Eq. (2.4)
    This restriction reduces the eight naive alignment possibilities to four, and is the basis for enumerating the six pairs in Section 3.
  • domain assumption chi_eff and kappa are constant on the precession timescale and vary only on the radiation-reaction timescale
    This constancy is used in Eqs. (3.1)-(3.2) to impose equality of these quantities at the two endpoints.

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Pith. "Pith review of Coincident morphological transitions in precessing black-hole binaries." pith.science (2026). https://pith.science/paper/EZR4HNPA

@misc{pith2026250819735,
  author       = {Pith},
  title        = {Pith review of: Coincident morphological transitions in precessing black-hole binaries},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/EZR4HNPA}},
  note         = {Machine review of arXiv:2508.19735}
}
read the original abstract

We present new insights into the phenomenology of post-Newtonian spin precession in black-hole binaries. Using multi-timescale methods, previous work has shown that the precession and nutation dynamics in such systems can be classified into so-called spin morphologies --mutually exclusive regions that partition the configuration space and characterize the motion of the black-hole spins relative to the binary's angular momentum. Radiation reaction can induce secular transitions between different morphology classes, which are generic occurrences during the inspiral of black-hole binaries. In this contribution, we systematically explore a more restrictive class of solutions in which multiple morphological transitions occur concurrently, i.e., within the same precession cycle. We find that all such cases can be mapped and characterized analytically, and we confirm these findings through numerical integrations. These coincident transitions correspond to extreme spin configurations in black-hole binaries with potential observational signatures in gravitational-wave astronomy.

Figures

Figures reproduced from arXiv: 2508.19735 by the authors.

Figure 1
Figure 1. Fraction f of BH binaries in each of the four spin morphologies: L0 (blue), Lπ (red), C+ (green), and C− (yellow). We consider a set of 106 sources with q = 0.99, χ1 = 0.5, χ1 = 1, and isotropic spin orientations. The vertical dashed line indicates the critical r = rwide from Eq. (3.4) where the C− morphology becomes accessible. These binaries are initialized with isotropic spin directions at r = ∞ and evolved down … view at source ↗
Figure 2
Figure 2. Precession-averaged evolution of the tilt angles [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗

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Works this paper leans on

43 extracted references · 14 canonical work pages

  1. [1]

    T. A. Apostolatos, C. Cutler, G. J. Sussman, and K. S. Thorne, Spin-induced orbital precession and its modulation of the gravitational waveforms from merging binaries, Phys. Rev. D 49, 6274 (1994)

    work page 1994

  2. [2]

    A. G. Abac et al., GWTC-4.0: Population Properties of Merging Compact Binaries, (2025), arXiv:2508.18083 [astro-ph.HE]

    arXiv 2025

  3. [3]

    Colpi et al., LISA Definition Study Report, ESA-SCI-DIR-RP-002 (2024), arXiv:2402.07571 [astro-ph.CO]

    M. Colpi et al., LISA Definition Study Report, ESA-SCI-DIR-RP-002 (2024), arXiv:2402.07571 [astro-ph.CO]

    arXiv 2024

  4. [4]

    Mandel and A

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

    arXiv 2022

  5. [5]

    Mapelli, Formation Channels of Single and Binary Stellar-Mass Black Holes, in Handbook of Gravitational Wave Astronomy(Springer, 2021) p

    M. Mapelli, Formation Channels of Single and Binary Stellar-Mass Black Holes, in Handbook of Gravitational Wave Astronomy(Springer, 2021) p. 16, 2106.00699 [astro-ph.HE]

    arXiv 2021

  6. [6]

    Black hole science with the Laser Interferometer Space Antenna

    A. Sesana, Black hole science with the Laser Interferometer Space Antenna, Front. Astron. Space Sci. 8, 7 (2021), arXiv:2105.11518 [astro-ph.CO]

    work page Pith review arXiv 2021

  7. [7]

    Amaro-Seoane et al., Astrophysics with the Laser Interferometer Space An- tenna, Living Rev

    P. Amaro-Seoane et al., Astrophysics with the Laser Interferometer Space An- tenna, Living Rev. Relativ. 26, 2 (2023), arXiv:2203.06016 [gr-qc]

    arXiv 2023

  8. [8]

    Gerosa and E

    D. Gerosa and E. Berti, Are merging black holes born from stellar collapse or previous mergers?, Phys. Rev. D 95, 124046 (2017), arXiv:1703.06223 [gr-qc]

    arXiv 2017

Show all 43 references
  1. [9]

    Fishbach, D

    M. Fishbach, D. E. Holz, and B. F arr, Are LIGO’s Black Holes Made from Smaller Black Holes?, Astrophys. J. Lett. 840, L24 (2017), arXiv:1703.06869 [astro-ph.HE]

    2017 arXiv

  2. [10]

    Gerosa and M

    D. Gerosa and M. Fishbach, Hierarchical mergers of stellar-mass black holes and their gravitational-wave signatures, Nat. Astron. 5, 749 (2021), arXiv:2105.03439 [astro-ph.HE]

    2021 arXiv

  3. [11]

    P. C. Peters, Gravitational Radiation and the Motion of Two Point Masses, Phys. Rev. 136, 1224 (1964)

    1964

  4. [12]

    Gerosa, M

    D. Gerosa, M. Kesden, U. Sperhake, E. Berti, and R. O’Shaughnessy, Multi- timescale analysis of phase transitions in precessing black-hole binaries, Phys. Rev. D 92, 064016 (2015), arXiv:1506.03492 [gr-qc]

    2015 arXiv

  5. [13]

    Klein, EFPE: Efficient fully precessing eccentric gravitational waveforms for binaries with long inspirals, (2021), arXiv:2106.10291 [gr-qc]

    A. Klein, EFPE: Efficient fully precessing eccentric gravitational waveforms for binaries with long inspirals, (2021), arXiv:2106.10291 [gr-qc]

    2021 arXiv

  6. [14]

    Gerosa, G

    D. Gerosa, G. Fumagalli, M. Mould, G. Cavallotto, D. P. Monroy, D. Gan- gardt, and V. De Renzis, Efficient multi-timescale dynamics of precessing black- hole binaries, Phys. Rev. D 108, 024042 (2023), arXiv:2304.04801 [gr-qc]

    2023 arXiv

  7. [15]

    J. D. Schnittman, Spin-orbit resonance and the evolution of compact binary sys- tems, Phys. Rev. D 70, 124020 (2004), arXiv:astro-ph/0409174 [astro-ph]

    2004 arXiv

  8. [16]

    Kesden, U

    M. Kesden, U. Sperhake, and E. Berti, Final spins from the merger of precessing binary black holes, Phys. Rev. D 81, 084054 (2010), arXiv:1002.2643 [astro-ph.GA]

    2010 arXiv

  9. [17]

    A. C. M. Correia, Cassini states for black hole binaries, Mon. Not. R. Astron. Soc. 457, L49 (2016), arXiv:1511.01890 [gr-qc]

    2016 arXiv

  10. [18]

    Gerosa, M

    D. Gerosa, M. Kesden, R. O’Shaughnessy, A. Klein, E. Berti, U. Sperhake, and D. Trifir`o, Precessional Instability in Binary Black Holes with Aligned Spins, Phys. Rev. Lett. 115, 141102 (2015), arXiv:1506.09116 [gr-qc]

    2015 arXiv

  11. [19]

    C. O. Lousto and J. Healy, Unstable flip-flopping spinning binary black holes, Phys. Rev. D 93, 124074 (2016), arXiv:1601.05086 [gr-qc]. Coincident morphological transitions in precessing black-hole binaries 13

    2016 arXiv

  12. [20]

    Mould and D

    M. Mould and D. Gerosa, Endpoint of the up-down instability in precessing binary black holes, Phys. Rev. D 101, 124037 (2020), arXiv:2003.02281 [gr-qc]

    2020 arXiv

  13. [21]

    X. Zhao, M. Kesden, and D. Gerosa, Nutational resonances, transitional preces- sion, and precession-averaged evolution in binary black-hole systems, Phys. Rev. D 96, 024007 (2017)

    2017

  14. [22]

    Gerosa, A

    D. Gerosa, A. Lima, E. Berti, U. Sperhake, M. Kesden, and R. O’Shaughnessy, Wide nutation: binary black-hole spins repeatedly oscil- lating from full alignment to full anti-alignment, Class. Quantum Grav. 36, 105003 (2019), arXiv:1811.05979 [gr-qc]

    2019 arXiv

  15. [23]

    C. O. Lousto, J. Healy, and H. Nakano, Spin flips in generic black hole binaries, Phys. Rev. D 93, 044031 (2016), arXiv:1506.04768 [gr-qc]

    2016 arXiv

  16. [24]

    S. Khan, K. Chatziioannou, M. Hannam, and F. Ohme, Phenomenological model for the gravitational-wave signal from precessing binary black holes with two-spin effects, Phys. Rev. D 100, 024059 (2019), arXiv:1809.10113 [gr-qc]

    2019 arXiv

  17. [25]

    Pratten, S

    G. Pratten, S. Husa, C. Garc´ıa-Quir´os, M. Colleoni, A. Ramos-Buades, H. Estell´es, and R. Jaume, Setting the cornerstone for a family of models for gravitational waves from compact binaries: The dominant harmonic for nonprecess- ing quasicircular black holes, Phys. Rev. D 10...

    2020 arXiv

  18. [26]

    Kesden, D

    M. Kesden, D. Gerosa, R. O’Shaughnessy, E. Berti, and U. Sperhake, Effective Potentials and Morphological Transitions for Binary Black Hole Spin Precession, Phys. Rev. Lett. 114, 081103 (2015), arXiv:1411.0674 [gr-qc]

    2015 arXiv

  19. [27]

    Racine, Analysis of spin precession in binary black hole systems including quadrupole-monopole interaction, Phys

    ´E. Racine, Analysis of spin precession in binary black hole systems including quadrupole-monopole interaction, Phys. Rev. D 78, 044021 (2008), arXiv:0803.1820 [gr-qc]

    2008 arXiv

  20. [28]

    Gerosa et al

    D. Gerosa et al. , precession, github.com/dgerosa/precession, doi.org/10.5281/zenodo.1478928 (2023)

    2023 doi

  21. [29]

    N. K. Johnson-McDaniel, S. Kulkarni, and A. Gupta, Inferring spin tilts at formation from gravitational wave observations of binary black holes: Interfacing precession-averaged and orbit-averaged spin evolution, Phys. Rev. D 106, 023001 (2022), arXiv:2107.11902 [astro-ph.HE]

    2022 arXiv

  22. [30]

    H. Yu, S. Ma, M. Giesler, and Y. Chen, Spin and eccentricity evolution in triple systems: From the Lidov-Kozai interaction to the final merger of the inner binary, Phys. Rev. D 102, 123009 (2020), arXiv:2007.12978 [gr-qc]

    2020 arXiv

  23. [31]

    Fumagalli and D

    G. Fumagalli and D. Gerosa, Spin-eccentricity interplay in merging binary black holes, Phys. Rev. D 108, 124055 (2023), arXiv:2310.16893 [gr-qc]

    2023 arXiv

  24. [32]

    Singh, N

    A. Singh, N. K. Johnson-McDaniel, A. Gupta, and K. S. Phukon, Tracing the evolution of eccentric precessing binary black holes: a hybrid approach, (2025), arXiv:2505.07238 [astro-ph.HE]

    2025 arXiv

  25. [33]

    LaHaye, H

    M. LaHaye, H. Yang, B. Bonga, and Z. Lyu, Efficient fully precessing gravita- tional waveforms for binaries with neutron stars, Phys. Rev. D 108, 043018 (2023), arXiv:2212.04657 [gr-qc]

    2023 arXiv

  26. [34]

    Gerosa, U

    D. Gerosa, U. Sperhake, and J. Voˇsmera, On the equal-mass limit of precessing black-hole binaries, Class. Quantum Grav. 34, 064004 (2017), arXiv:1612.05263 [gr- qc]

    2017 arXiv

  27. [35]

    Yunes and E

    N. Yunes and E. Berti, Accuracy of the post-Newtonian approximation: Optimal asymptotic expansion for quasicircular, extreme-mass ratio inspirals, Phys. Rev. D 77, 124006 (2008), arXiv:0803.1853 [gr-qc]. 14 Gerosa, Foroni, Fumagalli, Berti

    2008 arXiv

  28. [36]

    Zhang, N

    Z. Zhang, N. Yunes, and E. Berti, Accuracy of the post-Newtonian approxi- mation. II. Optimal asymptotic expansion of the energy flux for quasicircular, ex- treme mass-ratio inspirals into a Kerr black hole, Phys. Rev. D 84, 024029 (2011), arXiv:1103.6041 [gr-qc]

    2011 arXiv

  29. [37]

    V arma, M

    V. V arma, M. Mould, D. Gerosa, M. A. Scheel, L. E. Kidder, and H. P. Pfeif- fer, Up-down instability of binary black holes in numerical relativity, Phys. Rev. D 103, 064003 (2021), arXiv:2012.07147 [gr-qc]

    2021 arXiv

  30. [38]

    De Renzis, D

    V. De Renzis, D. Gerosa, M. Mould, R. Buscicchio, and L. Zanga, Parameter estimation of binary black holes in the endpoint of the up-down instability, Phys. Rev. D 108, 024024 (2023), arXiv:2304.13063 [gr-qc]

    2023 arXiv

  31. [39]

    Gangardt, D

    D. Gangardt, D. Gerosa, M. Kesden, V. De Renzis, and N. Steinle, Constrain- ing black-hole binary spin precession and nutation with sequential prior conditioning, Phys. Rev. D 106, 024019 (2022), arXiv:2204.00026 [gr-qc]

    2022 arXiv

  32. [40]

    N. K. Johnson-McDaniel, K. S. Phukon, N. V. Krishnendu, and A. Gupta, Distinguishing binary black hole precessional morphologies with gravitational wave observations, Phys. Rev. D 108, 103003 (2023), arXiv:2301.10125 [astro-ph.HE]

    2023 arXiv

  33. [41]

    Biscoveanu, Probing Spin-Orbit Resonances with the Binary Black Hole Popu- lation, (2025), arXiv:2502.04278 [astro-ph.HE]

    S. Biscoveanu, Probing Spin-Orbit Resonances with the Binary Black Hole Popu- lation, (2025), arXiv:2502.04278 [astro-ph.HE]

    2025 arXiv

  34. [42]

    V arma, S

    V. V arma, S. Biscoveanu, M. Isi, W. M. F arr, and S. Vitale, Hints of Spin-Orbit Resonances in the Binary Black Hole Population, Phys. Rev. Lett. 128, 031101 (2022), arXiv:2107.09693 [astro-ph.HE]

    2022 arXiv

  35. [43]

    G. Occhialini

    D. Gerosa, M. Kesden, E. Berti, R. O’Shaughnessy, and U. Sperhake, Resonant-plane locking and spin alignment in stellar-mass black-hole binaries: A diagnostic of compact-binary formation, Phys. Rev. D 87, 104028 (2013), arXiv:1302.4442 [gr-qc] [Gerosa, Foroni, Fumagalli] Dipar...

    2013 arXiv

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