REVIEW 2 major objections 5 minor 66 references
Scalar kicks and memory
T0 review · 2 major / 5 minor · reviewed 2026-08-11 · deepseek-v4-flash
Pith's one-line read The central claim is that disformal scalar couplings leave no trace in linear memory or zero-frequency power, while conformal couplings change both, so kicks are the only disformal messenger.
desk verdict A clean separation between conformal memory and disformal kicks, but the kick formula has a factor-of-2 error that needs fixing before the numbers are trusted. read the letter →
The pith
A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.
The reading
What carries the argument
The machinery is the long-wavelength effective action for the radiative fields, $S_{\rm eff} = S_0 + S_1 + S_2 + S_{\rm NL}$, in which the binary is collapsed to multipole moments of an effective source $J = J_{\rm con} + J_{\rm dis}$. From these moments one builds the scalar wave's effective charge $Q(t_R) = I_\phi + N_i \dot I^i_\phi + \tfrac12 N_i N_j \ddot I^{ij}_\phi$, whose monopole, dipole and quadrupole moments drive the scalar field at large distance. The memory is computed through the Jacobi equation in the Jordan metric, where the scalar contributes a conformal linear term, a disformal non-linear term quadratic in $\phi$, and the direct Jordan displacement; the disformal terms cancel after the two time integrations. The key structural fact is that the disformal source moment is proportional to $d^2/dt^2(1/r)$, whose Fourier transform behaves logarithmically near $\omega = 0$ and therefore drops out of the zero-frequency limits that define memory and power, while it survives in the momentum flux that produces kicks.
What would settle it
Extend the effective action to order $\Lambda^{-4}$, including the scalar dipole moment $I^i_\phi$ that was dropped, and recompute the double-time-integrated Jordan displacement and the limit $\omega^3 \tilde I^{ij}_\phi(\omega)$ as $\omega \to 0$; if either receives a non-vanishing contribution proportional to $1/\Lambda^4$, the disformal memory is not exactly zero. Observationally, a hyperbolic compact-binary event in which the inferred memory amplitude depends on the disformal scale $\Lambda$, or in which the measured kick is inconsistent with $\Delta V^y_\phi = v_{\rm cm} \epsilon_\Lambda f^y_\phi(e)$, would also falsify the central claim.
Extended reading notes
Core claim
On its own terms, the paper's central result is that in a scalar-tensor theory whose Jordan metric is $g^J_{\mu\nu} = A^2(\phi) g_{\mu\nu} + 2 \Lambda^{-2} m_{\rm Pl}^{-2} \partial_\mu\phi \partial_\nu\phi$, the scalar linear memory of a hyperbolic binary receives contributions from conformal and disformal terms that exactly cancel in the disformal channel: the total scalar displacement is $\delta = 2 G_N \beta (1 - (\vec N \cdot \hat\ell)^2)/R \, [Q(+\infty) - Q(-\infty)]$, with the disformal pieces of the Jordan displacement and of the non-linear memory cancelling each other. Equivalently, the scalar power spectrum at zero frequency receives only a conformal quadrupole contribution, giving $P^{(Q)}_\phi(0) = (\beta^2/3) P_{\rm GW}(0)$, while the monopole vanishes at $\omega = 0$ and the disformal quadrupole term vanishes logarithmically. By contrast, the recoil of the centre of mass is set by the combination $\epsilon_\Lambda = \beta^2 G_N m/(\Lambda^2 p^3)$, giving $\Delta V^y_\phi = v_{\rm cm} \epsilon_\Lambda f^y_\phi(e)$, where $f^y_\phi$ grows as $e^8$ at large eccentricity. The paper therefore claims that disformal couplings are observable through kicks, not through memory, making the two couplings experimentally separable.
Load-bearing premise
The calculation assumes the derivative expansion of the scalar effective action can be cut at second order and at leading order in the disformal coupling $1/\Lambda^2$, and that scalar dipole radiation at order $1/\Lambda^4$ is negligible in the zero-frequency limits that define memory and power.
Editorial extensions
If this is right
- A measurement of scalar linear memory in a hyperbolic binary fixes the conformal coupling $\beta$, independent of the disformal scale $\Lambda$.
- A measurement of the scalar kick fixes the dimensionless combination $\epsilon_\Lambda = \beta^2 G_N m/(\Lambda^2 p^3)$, so combining memory and kick data separates $\beta$ from $\Lambda$.
- The low-frequency scalar power spectrum carries the same conformal information as memory, so comparing $P_\phi(0)$ with the GR spectrum tests whether a scalar is present.
- In a conformal-only theory the GR memory-power relation is modified by the factor $\beta^2$, so detecting a deviation from the GR relation is an indicator of conformal scalar radiation.
- Because the scalar kick grows as $e^8$ while the GR kick grows as $e^4$ in eccentricity, highly eccentric hyperbolic encounters are the best place to look for disformal effects.
Reading between the lines
- The cancellation that makes disformal memory vanish may be an accident of the leading-order derivative expansion; testing whether it persists at order $\Lambda^{-4}$ would reveal whether the conformal/disformal separation is exact or approximate.
- If white-dwarf environments indeed allow a lighter $\Lambda$ than neutron stars, hyperbolic white-dwarf binaries become a natural laboratory: memory would provide $\beta$ and the kick would provide $\Lambda$ from the same source class.
- The result suggests a selection rule worth checking: zero-frequency radiation observables such as memory and $P(0)$ may be blind to derivative couplings whose source terms are total time derivatives falling faster than $1/t$, while momentum-flux observables remain sensitive to them.
- Extending the calculation to bound orbits or eccentric inspirals, where kicks and memory accumulate over many cycles, could make the $e^8$ eccentricity enhancement even more pronounced.
Editorial analysis
A structured set of objections, weighed in public.
Referee Report
Summary. This paper studies scalar-tensor theories in which a massless scalar couples conformally (β) and disformally (Λ) to matter, focusing on hyperbolic binary orbits. It derives the 1PN conservative dynamics and the resulting precession, then turns to radiative effects: the scalar contribution to the linear memory effect (through the Jordan metric and the Jacobi equation) and the scalar contribution to the centre-of-mass kick. The central claims are that the disformal interaction cancels in the scalar memory and in the zero-frequency emitted power spectrum, that the conformal interaction modifies the GR linear memory and the quadrupole power spectrum at zero frequency (thereby breaking the GR memory-power spectrum relation), and that disformal interactions produce a centre-of-mass kick proportional to ϵ_Λ = β²G_N m/(Λ²p³). The paper also gives order-of-magnitude estimates for detectability, arguing that combined measurements of memory and kicks could disentangle β and Λ.
Significance. If the results hold, the paper provides a concrete observational strategy for separating conformal and disformal couplings of light scalars using gravitational-wave memory and recoil measurements on hyperbolic binaries. The zero-frequency power spectrum is derived twice, once from the memory formula and once from Hankel-function asymptotics in Appendix C, and the two agree; this is a strong internal consistency check. The manuscript also contains explicit closed-form expressions for the memory and kick as functions of eccentricity, which is valuable for future data-analysis applications. However, the central quantitative kick prediction contains an algebraic factor-of-two error in the dipole-quadrupole contribution, and the memory cancellation is only demonstrated at leading order in the EFT expansion; both points need attention before the claims are accepted at face value.
major comments (2)
- [V A, Eq. (155)] The dipole-quadrupole contribution to dP^i/dt carries a spurious factor of 2. From Eq. (102), \dot Q = \dot I_φ + N_i \ddot I^i_φ + (1/2)N_j N_k \dddot I^{jk}_φ, so the 2BC cross term in (\dot Q)^2 is N_j N_k N_l \ddot I^j_φ \dddot I^{kl}_φ with coefficient unity, not 2. Using ∫ dΩ N^i N^j N^k N^l = (4π/15)(δ^{ij}δ^{kl}+δ^{ik}δ^{jl}+δ^{il}δ^{jk}) and tracelessness of \dddot I^{kl}_φ gives ∫ dΩ N^i (\dot Q)^2 ⊃ (8π/15) \ddot I^j_φ \dddot I^{ij}_φ, which with the prefactor in Eq. (154) yields −4G_N/15, not −8G_N/15. This factor propagates into Eq. (157), Eq. (D12), and the final kick function f^y_φ(e) in Eq. (D18), changing the numerical prediction for ΔV^y_φ. The memory result is unaffected, but the quantitative kick prediction must be corrected by re-deriving the coefficients in Appendix D.
- [IV A-C, Eq. (132)] The abstract and conclusions state that 'the disformal interaction does not contribute to the memory effect', but the calculation demonstrates this only at leading order in the disformal expansion and at second order in derivatives. The source moments in Eqs. (95)-(99), the Jordan metric in Eq. (104), and the effective charge in Eq. (102) are all truncated at O(1/Λ²), and the cancellation between Eqs. (123) and (131) uses exactly these leading-order pieces. The manuscript itself notes after Eq. (137) that the scalar dipole appears at 1/Λ⁴ and is neglected, so the result does not exclude 1/Λ⁴ or higher-derivative disformal contributions to the double-time-integrated displacement. Please either prove the cancellation beyond leading order or qualify the central claim as holding at leading order in the EFT expansion.
minor comments (5)
- [IV B, Eq. (122)] In Eq. (122), the second term on the right-hand side is written with ∂_i ¯φ ∂_i ¯φ (both indices i), but to match the left-hand side h^φ_{ij} and the preceding Eq. (107) it should be ∂_i ¯φ ∂_j ¯φ.
- [Introduction] In the first paragraph, 'Hornesdki' should be 'Horndeski'.
- [Appendix D, Eq. (D4)] The notation '− 2 4G_N/15' in Eq. (D4) is ambiguous; it should be written with parentheses, e.g., −(8G_N/15) \ddot I^j_φ \dddot I^{ij}_φ.
- [Fig. 2] The axis labels and caption of Figure 2 appear corrupted in the source text (unresolved unicode tokens such as '˜/uni03C9'); the published figure should be regenerated with proper notation.
- [IV D, Eq. (145)] In Eq. (145), the ratio \bar P^{(M)}_φ / P_GW(0) compares the monopole normalization at ω ≪ Λ with the quadrupole zero-frequency spectrum; please state explicitly that this is a comparison of normalization factors rather than of the full frequency-dependent spectra, and define r_min in the denominator.
Circularity Check
No significant circularity: the memory and kick results are new integrals over the same scalar charge Q, not restatements of its definition.
full rationale
The central memory result (Eq. 132) is obtained by adding three explicitly computed contributions: the Jordan displacement (Eq. 123), the linear conformal memory (Eq. 129), and the non-linear disformal memory (Eq. 131). The disformal pieces in Eqs. (123) and (131) are opposite in sign and cancel; the surviving term is proportional to beta [Q(+infinity)-Q(-infinity)]. This is an algebraic cancellation, not an input assumption. The kick result (Eq. 160) follows from a separate momentum-flux integral (Eqs. 152-155) evaluated in Appendix D; the proportionality to epsilon_Lambda is a consequence of the 1/Lambda^2 source moments, and the eccentricity function f^y_phi(e) is a new calculation rather than a fitted parameter. The 1PN Fock action (Eq. 65) and the scalar source moments (Eqs. 95-99) are taken from earlier work [7, 50, 55], but they are parameter-free starting inputs with stated ordering assumptions (1PN, leading order in Lambda^-2 and in derivatives), and neither contains the memory or kick formulas. No parameter is fitted to data and renamed a prediction; no uniqueness theorem is imported from the authors to force a choice; and the disformal precession comparison in Sec. III D explicitly corrects earlier results [13, 52] rather than relying on them as black boxes. The truncation at second order in derivatives and the neglect of the 1/Lambda^4 dipole force are acknowledged assumptions (Sec. IV A, after Eq. 137); they limit the regime of validity but do not make the derivation circular. A possible arithmetic factor in Eq. (155) would affect the quantitative kick prediction but is a correctness issue, not a circularity issue.
Assumptions & free parameters
free parameters (2)
- beta (conformal coupling)
- Lambda (disformal suppression scale)
assumptions (5)
- domain assumption The scalar field is massless and its equation of motion is linear, sourced only by matter T_mu_nu (Eq. 47).
- domain assumption Matter is universally coupled to the Jordan metric gJ_mu_nu = A^2(phi)g_mu_nu + 2/(Lambda^2 m_Pl^2) partial_mu phi partial_nu phi (Eq. 45), and detectors respond to this Jordan frame metric in the Jacobi equation (105).
- standard math The 1PN Fock/EIH action, Eq. (65), and the radiation source multipoles I_phi, I^i_phi, I^ij_phi, Eqs. (95)-(99), are taken from the authors' prior work [7,50,55].
- domain assumption The binary is in a weak-field 1PN regime with hyperbolicity e > 1, no spins, and closest approach large enough for PN methods (Secs. II C and III).
- standard math Standard Hankel integral representations and recursion relations used in Appendices B and C are correct.
Cite this review
Pith. "Pith review of Scalar kicks and memory." pith.science (2026). https://pith.science/paper/WTOI7O4A
@misc{pith2026241217938,
author = {Pith},
title = {Pith review of: Scalar kicks and memory},
year = {2026},
howpublished = {\url{https://pith.science/paper/WTOI7O4A}},
note = {Machine review of arXiv:2412.17938}
}
read the original abstract
A scalar field coupled conformally and disformally to matter affects both the linear memory effect for binary systems on hyperbolic orbits, as well as the kick velocity for binaries on bound or unbound orbits. We study these corrections in detail, their order of magnitude, and discuss their detectability. In particular, we find that the disformal interaction does not contribute to the memory effect and the emitted power spectrum at zero frequency. The conformal interaction corrects the GR linear memory and the quadrupole emitted power at zero frequency resulting in a breaking of the GR memory-power spectrum relationship. On the other hand, disformal interactions give rise to a change of momentum for the centre of mass. Hence, measuring both the linear memory effect and the kicks for hyperbolic orbits would give access to the conformal and disformal couplings of nearly massless scalars to matter.
Figures
Reference graph
Works this paper leans on
-
[1]
In the quadrupole approximation (see e.g
Linear memory and energy spectrum The linear memory effect is a non-zero change in the 3D transverse and traceless (TT) metric perturbation between t = ±∞, and leads to a permanent displacement δL/L in the arm lengths of a GW interferometer. In the quadrupole approximation (see e.g. [33]) hij(t, ⃗R) = 2GN c4R Λij,kℓ( ⃗N ) ¨I kℓ(tR) (13) where R is the dis...
-
[2]
Linear memory effects for hyperbolic orbits We now focus on binary system whose orbits are hyperbolic. Calculation of PGW(ω) (see below) shows that a short GW burst of characteristic frequency ωmax ∼ 6 s GN m r3 min √e − 1 e + 1 is emitted near rmin with a corresponding linear memory effect ∆ hij ̸= 0. Depending on m, eand rmin ≫ rs ≡ 2Gm, this characteri...
-
[3]
should also couple to matter 1. These couplings are problematic in the solar system where tests of gravitational interactions are very precise, ranging from the Cassini probe of the Shapiro delay [4] to the Microscope test of the equivalence principle [5, 6]. They could also be a blessing as they could open a wealth of new phenomena to observations, for i...
arXiv 2025
-
[4]
Bertotti, L
B. Bertotti, L. Iess, and P. Tortora, Nature 425, 374 (2003)
2003
-
[5]
(113) 16 There is a linear scalar memory effect (denoted by L) δξ i L = − β mPl ∂i∂j Z t −∞ dτ Z τ −∞ dτ ′ ¯ϕ(x, τ′) ξj 0 (114) which depends on the conformal coupling β as well as a non-linear scalar memory effect (denoted by NL) depending quadratically on the history of the scalar field δξ i N L= − Z t −∞ dτ Z τ −∞ dτ ′ 1 m2 PlΛ2 2(∂i∂j ¯ϕ)(∂2 0 ¯ϕ) + ∂...
-
[6]
(115) These are particular to the presence of couplings between matter and the scalar field. Notice that this non-linear effect comes from the disformal coupling which is quadratic in the scalar field and differs from a potential non-linear effect of the scalar in the scalar field equation. As already mentioned, only the matter energy-momentum tensor acts...
-
[7]
17 a small contribution as β2 <∼ 2.1 · 10−5
When solar system tests are considered, the Cassini bound leads to 10 Non-linear effects in the scalar field equation would appear if the scalar has self-interactions which are not taken into account here. 17 a small contribution as β2 <∼ 2.1 · 10−5. On the other hand in the vicinity of compact objects, scalarisation could take place with β = O(1). The di...
-
[8]
Appendix D: Calculation of the Scalar momentum force The following identities will be useful
See section II B 2 for further discussion. Appendix D: Calculation of the Scalar momentum force The following identities will be useful. From Newton’s law to lowest order ⃗ a= −Geff N mr−3⃗ r, one has d2 dt2 1 r = 3 r5 (⃗ r· ⃗ v)2 − v2 r3 + Geff N m r4 (D1) d3 dt3 1 r = − 15 r7 (⃗ r· ⃗ v)3 + 9 r5 (⃗ r· ⃗ v)v2 − 8Geff N m r6 (⃗ r· ⃗ v) (D2) d4 dt4 1 r = 75...
work page 2016
Show all 66 references
- [9]
-
[10]
E. J. Copeland, M. Sami, and S. Tsujikawa, Int. J. Mod. Phys. D 15, 1753 (2006), hep-th/0603057
2006 arXiv
-
[11]
P. Brax, S. Casas, H. Desmond, and B. Elder, Universe 8, 11 (2021), 2201.10817
2021 arXiv
-
[13]
Berg´ e, P
J. Berg´ e, P. Brax, G. M´ etris, M. Pernot-Borr` as, P. Touboul, and J.-P. Uzan, Phys. Rev. Lett. 120, 141101 (2018), 1712.00483
2018 arXiv
-
[14]
Touboul et al
P. Touboul et al. (MICROSCOPE), Phys. Rev. Lett. 129, 121102 (2022), 2209.15487
2022 arXiv
-
[15]
Brax, A.-C
P. Brax, A.-C. Davis, and A. Kuntz, Phys. Rev. D 99, 124034 (2019), 1903.03842
2019 arXiv
-
[16]
C. M. Will, Living Rev. Rel. 17, 4 (2014), 1403.7377
2014 arXiv
- [17]
- [18]
- [19]
-
[20]
Mukhopadhyay, C
M. Mukhopadhyay, C. Cardona, and C. Lunardini, JCAP 07, 055 (2021), 2105.05862
2021 arXiv
-
[22]
Brax, A.-C
P. Brax, A.-C. Davis, S. Melville, and L. K. Wong, JCAP 03, 001 (2021), 2011.01213
2021 arXiv
-
[23]
Abbott et al
R. Abbott et al. (LIGO Scientific, Virgo), Astrophys. J. Lett. 900, L13 (2020), 2009.01190
2020
-
[24]
Ranjan, K
S. Ranjan, K. Jani, A. H. Nitz, K. Holley-Bockelmann, and C. Cutler (2024), 2406.11926
2024 arXiv
-
[25]
Healy, F
J. Healy, F. Herrmann, I. Hinder, D. M. Shoemaker, P. Laguna, and R. A. Matzner, Phys. Rev. Lett. 102, 041101 (2009), URL https://link.aps.org/doi/10.1103/PhysRevLett.102.041101
2009 doi
- [26]
-
[27]
P. Brax, C. Burrage, and C. Englert, Phys. Rev. D 92, 044036 (2015), 1506.04057
2015 arXiv
- [28]
- [29]
-
[30]
Inchausp´ e, S
H. Inchausp´ e, S. Gasparotto, D. Blas, L. Heisenberg, J. Zosso, and S. Tiwari (2024), 2406.09228
2024 arXiv
-
[31]
Goncharov, L
B. Goncharov, L. Donnay, and J. Harms, Phys. Rev. Lett. 132, 241401 (2024), 2310.10718
2024 arXiv
-
[32]
Gasparotto, R
S. Gasparotto, R. Vicente, D. Blas, A. C. Jenkins, and E. Barausse, Phys. Rev. D 107, 124033 (2023), 2301.13228
2023 arXiv
-
[33]
Heisenberg, N
L. Heisenberg, N. Yunes, and J. Zosso, Phys. Rev. D 108, 024010 (2023), 2303.02021
2023 arXiv
-
[34]
Tahura, D
S. Tahura, D. A. Nichols, A. Saffer, L. C. Stein, and K. Yagi, Phys. Rev. D 103, 104026 (2021), 2007.13799
2021 arXiv
- [35]
-
[36]
Kerachian, S
M. Kerachian, S. Mukherjee, G. Lukes-Gerakopoulos, and S. Mitra, Astron. Astrophys. 684, A17 (2024), 2311.16634
2024 arXiv
-
[37]
V. B. Braginsky and K. S. Thorne, Nature (London) 327, 123 (1987)
1987
-
[38]
Poisson and C
E. Poisson and C. M. Will, Gravity: Newtonian, Post-Newtonian, Relativistic (Cambridge University Press, 2014)
2014
-
[39]
Damour and N
T. Damour and N. Deruelle, Annales de l’I.H.P. Physique th´ eorique 43, 107 (1985), URL http://eudml.org/doc/76291
1985
-
[40]
Caldarola, S
M. Caldarola, S. Kuroyanagi, S. Nesseris, and J. Garcia-Bellido (2023), 2307.00915
2023 arXiv
-
[41]
Maggiore, Gravitational Waves
M. Maggiore, Gravitational Waves. Vol. 1: Theory and Experiments (Oxford University Press, 2007), ISBN 978-0-19- 171766-6, 978-0-19-852074-0
2007
-
[42]
S. Bini, S. Tiwari, Y. Xu, L. Smith, M. Ebersold, G. Principe, M. Haney, P. Jetzer, and G. A. Prodi, Phys. Rev. D 109, 042009 (2024), 2311.06630
2024 arXiv
-
[43]
Garc ´ ıa-Bellido, S
J. Garc ´ ıa-Bellido, S. Jaraba, and S. Kuroyanagi, Phys. Dark Univ.36, 101009 (2022), 2109.11376
2022 arXiv
- [44]
-
[45]
A. Hait, S. Mohanty, and S. Prakash, Phys. Rev. D 109, 084037 (2024), 2211.13120
2024 arXiv
-
[46]
Gr¨ obner, P
M. Gr¨ obner, P. Jetzer, M. Haney, S. Tiwari, and W. Ishibashi, Class. Quant. Grav. 37, 067002 (2020), 2001.05187
2020 arXiv
-
[47]
Blanchet and G
L. Blanchet and G. Sch¨ afer, Monthly Notices of the Royal Astronomical Society 239, 845 (1989), ISSN 0035-8711, https://academic.oup.com/mnras/article-pdf/239/3/845/18194791/mnras239-0845.pdf, URL https://doi.org/10.1093/ mnras/239.3.845
1989
-
[48]
De Vittori, P
L. De Vittori, P. Jetzer, and A. Klein, Phys. Rev. D 86, 044017 (2012), 1207.5359
2012 arXiv
-
[49]
I. S. Gradshteyn, I. M. Ryzhik, D. Zwillinger, and V. Moll, Table of integrals, series, and products; 8th ed. (Academic Press, Amsterdam, 2015)
2015
-
[50]
Merritt, M
D. Merritt, M. Milosavljevic, M. Favata, S. A. Hughes, and D. E. Holz, Astrophys. J. Lett. 607, L9 (2004), astro- ph/0402057
2004
-
[51]
M. J. Fitchett, Monthly Notices of the Royal Astronomical Society 203, 1049 (1983), ISSN 0035- 8711, https://academic.oup.com/mnras/article-pdf/203/4/1049/18223796/mnras203-1049.pdf, URL https://doi.org/ 10.1093/mnras/203.4.1049
1983 doi
-
[52]
by first considering ϕ(0) = − β mPl □−1T (49) where the retarded Green’s function is selected. The disformal interaction is taken into account in a ladder expansion ϕ = ϕ(0) + δϕ where δϕ = ∞X n=0 δϕ(n) (50) with □δϕ(0) = 2 Λ2m2 Pl (Dµ∂νϕ(0))T µν (51) □δϕ(n+1) = 2 Λ2m2 Pl (Dµ∂...
-
[53]
J. G. Baker, J. Centrella, D.-I. Choi, M. Koppitz, J. R. van Meter, and M. C. Miller, Astrophys. J. Lett. 653, L93 (2006), astro-ph/0603204
2006 arXiv
-
[54]
J. D. Schnittman and A. Buonanno, The Astrophysical Journal 662, L63 (2007), URL https://dx.doi.org/10.1086/ 519309
2007
-
[55]
Damour and G
T. Damour and G. Esposito-Farese, Class. Quant. Grav. 9, 2093 (1992)
1992
-
[56]
J. D. Bekenstein, Phys. Rev. D 48, 3641 (1993), gr-qc/9211017
1993 arXiv
- [57]
-
[59]
Deffayet, X
C. Deffayet, X. Gao, D. A. Steer, and G. Zahariade, Phys. Rev. D 84, 064039 (2011), 1103.3260
2011 arXiv
- [60]
-
[61]
D. L. Richardson and T. J. Kelly, in Long Term Evolution of Planetary Systems , edited by R. Dvorak and J. Henrard (Springer Netherlands, Dordrecht, 1988), pp. 193–210, ISBN 978-94-009-2285-3
1988
-
[62]
Benisty, P
D. Benisty, P. Brax, and A.-C. Davis, Phys. Rev. D 107, 064049 (2023), 2212.03098
2023 arXiv
- [63]
-
[64]
W. D. Goldberger and I. Z. Rothstein, Phys. Rev. D 73, 104029 (2006), hep-th/0409156
2006 arXiv
-
[65]
R. A. Porto, Phys. Rept. 633, 1 (2016), 1601.04914
2016 arXiv
- [66]
- [67]
-
[68]
F. M. Ramazano˘ glu and F. Pretorius, Phys. Rev. D 93, 064005 (2016), 1601.07475
2016 arXiv
-
[69]
Ashtekar, T
A. Ashtekar, T. De Lorenzo, and N. Khera, Phys. Rev. D 101, 044005 (2020), 1910.02907
2020 arXiv
Reviewed August 11, 2026 · model on record in the stance chip above.
Discussion (0). Continue with ORCID to comment.