pith. sign in

arxiv: 2606.00166 · v1 · pith:GYMSMWQ4new · submitted 2026-05-29 · 🌀 gr-qc

Cascading amplification of gravitational waves triggered by environment in dynamical Chern-Simons gravity

Han-Wen Hu , Chen Lan , Zong-Kuan Guo This is my paper

Pith reviewed 2026-06-28 21:34 UTC · model grok-4.3

classification 🌀 gr-qc
keywords dynamical Chern-Simons gravitygravitational wavesMathieu instabilityresonant cavityparametric amplificationblack holescalar perturbationsFloquet sidebands
0
0 comments X

The pith

An external oscillating environment triggers resonant amplification of gravitational waves in dynamical Chern-Simons gravity even at ultraweak coupling.

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

The paper examines how an external dynamical environment interacts with the dCS pseudoscalar field to amplify gravitational wave signals from black holes. The black hole barrier combined with an oscillating shell creates an effective resonant cavity that drives Mathieu instability in the scalar sector. Amplified scalar perturbations then act as a source for axial gravitational perturbations, producing a delayed secondary burst. This shows that small dCS corrections can build up through long-term parametric amplification and leave detectable imprints in gravitational wave signals.

Core claim

Within dynamical Chern-Simons gravity, the black hole barrier and external oscillating shell form an effective resonant cavity that triggers Mathieu instability in the dCS scalar sector. The optimal driving frequency is set by cavity length, while proximity to the horizon can suppress growth via leakage. In the frequency domain scalar perturbations show Floquet sidebands; in the time domain the amplified scalar sources axial gravitational perturbations and generates a delayed secondary burst. This establishes that dCS corrections at ultraweak coupling accumulate via long-term parametric amplification in a dynamical environment.

What carries the argument

The effective resonant cavity formed by the black hole barrier and external oscillating shell, which drives Mathieu instability in the pseudoscalar sector and cascades to gravitational waves.

If this is right

  • The optimal driving frequency for the instability equals the resonant cavity length.
  • Scalar perturbations develop Floquet sideband structures in the frequency domain.
  • Amplified scalars drive a delayed secondary burst in axial gravitational perturbations.
  • Leakage to the horizon creates a dynamical threshold when the environment lies too close to the black hole.

Where Pith is reading between the lines

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

  • The resonance mechanism suggests searching for sideband patterns or delayed bursts in gravitational wave data from black holes in oscillating environments such as accretion flows.
  • Similar cavity-like amplification could appear in other scalar-tensor theories when environmental oscillations are included.
  • Numerical relativity runs with explicit oscillating shells could directly test the predicted growth rates and thresholds.

Load-bearing premise

The external environment can be modeled as an oscillating shell that forms a resonant cavity with the black hole while linear perturbation theory remains valid without significant backreaction.

What would settle it

A simulation or observation showing absence of scalar growth, Floquet sidebands, or a delayed secondary gravitational wave burst when an oscillating shell is placed near a black hole would falsify the mechanism.

Figures

Figures reproduced from arXiv: 2606.00166 by Chen Lan, Han-Wen Hu, Zong-Kuan Guo.

Figure 1
Figure 1. Figure 1: FIG. 1: Logarithmic time-domain waveforms of the dCS scalar perturbation [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2: Two dimensional phase diagram of parametric resonance and the profile of the maximum Lyapunov [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3: Quantitative verification of the resonant geometric law. The relation between the extracted optimal [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4: Parametric resonance fingerprints and Floquet sidebands in the spectra of scalar perturbations [PITH_FULL_IMAGE:figures/full_fig_p010_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5: Panels (a) and (b) present the dynamical evolutions governed by the fully coupled perturbation equation (8) [PITH_FULL_IMAGE:figures/full_fig_p011_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6: Stability phase diagram and scaling laws of scalar-field parametric resonance [PITH_FULL_IMAGE:figures/full_fig_p021_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: FIG. 7: Two dimensional phase diagram and the corresponding ridge exponent for the four-point interaction. The [PITH_FULL_IMAGE:figures/full_fig_p025_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: FIG. 8: Verification of the cavity scaling for the four-point interaction. The vertical axis is the input [PITH_FULL_IMAGE:figures/full_fig_p025_8.png] view at source ↗
read the original abstract

Within the effective field theory framework of dynamical Chern-Simons (dCS) gravity, we investigate the cascading amplification mechanism of gravitational waves driven by an external dynamical environment. Considering the interaction between the environmental field and the dCS pseudoscalar, we find that the black hole barrier and the external oscillating shell collectively form an effective resonant cavity, which triggers Mathieu instability in the dCS scalar sector. Numerical results show that the optimal driving frequency is set by the length of the resonant cavity. When the environmental field lies too close to the black hole, leakage toward the event horizon suppresses the resonant growth, thus giving a dynamical threshold for the existence of the instability. In the frequency domain, scalar perturbations display the Floquet sideband structures. In the time domain, the amplified scalar field further acts as a source term to drive axial gravitational perturbations, generating a delayed secondary burst. This mechanism reveals that dCS corrections at ultraweak coupling can still accumulate via long-term parametric amplification in a dynamical environment, leaving discernible signatures in gravitational wave signals.

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 manuscript examines parametric amplification of the dCS pseudoscalar in the presence of a black hole and an external oscillating shell, which together form an effective resonant cavity. It reports that this setup triggers Mathieu instability, with numerical evolution yielding an optimal driving frequency set by cavity length, a leakage threshold near the horizon, Floquet sideband structure in the frequency domain, and a delayed secondary burst in axial gravitational perturbations sourced by the amplified scalar. The central claim is that ultraweak dCS couplings can accumulate observable signatures in GW signals via long-term environmental amplification.

Significance. If the linear-regime assumption holds, the work identifies a concrete mechanism by which small dCS corrections can be resonantly amplified in dynamical astrophysical environments, potentially producing detectable secondary GW features. The numerical demonstration of Floquet sidebands and the secondary burst constitutes a tangible advance in exploring modified-gravity effects beyond the weak-field limit.

major comments (2)
  1. [Numerical results (discussion of growth rate and leakage threshold)] The numerical results section does not compare the e-folding time of the reported Mathieu instability to the dynamical timescale of the shell or the metric; without this bound the fixed-background resonant-cavity assumption used to derive the instability remains unverified against backreaction.
  2. [Setup of the oscillating-shell model and linear perturbation equations] The perturbation equations are evolved on a fixed shell background; no estimate is given for the scalar energy density at which the sourced metric perturbations would alter the shell motion or invalidate the linear treatment, which is load-bearing for the claim that the instability persists long enough to produce a secondary burst.
minor comments (2)
  1. [Abstract] The abstract refers to 'cascading amplification' without a one-sentence definition; adding a brief parenthetical would improve readability.
  2. [Figures showing scalar perturbations] Figure captions for the frequency-domain plots should explicitly label the expected Floquet sideband spacing in terms of the driving frequency.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading of the manuscript and for highlighting the importance of verifying the linear-regime and fixed-background assumptions. We address each major comment below and have revised the manuscript to incorporate the requested comparisons and estimates.

read point-by-point responses

  1. Referee: [Numerical results (discussion of growth rate and leakage threshold)] The numerical results section does not compare the e-folding time of the reported Mathieu instability to the dynamical timescale of the shell or the metric; without this bound the fixed-background resonant-cavity assumption used to derive the instability remains unverified against backreaction.

    Authors: We agree that a direct comparison of timescales is required to substantiate the fixed-background assumption. In the revised manuscript we have added a dedicated paragraph in Section IV that extracts the e-folding time from the numerical growth curves and compares it to both the shell oscillation period and the light-crossing time of the resonant cavity. For the parameter values at which the instability is observed, the e-folding time is several shell periods, confirming that multiple amplification cycles occur before backreaction on the metric is expected to become appreciable. This addition directly addresses the concern. revision: yes

  2. Referee: [Setup of the oscillating-shell model and linear perturbation equations] The perturbation equations are evolved on a fixed shell background; no estimate is given for the scalar energy density at which the sourced metric perturbations would alter the shell motion or invalidate the linear treatment, which is load-bearing for the claim that the instability persists long enough to produce a secondary burst.

    Authors: We acknowledge the need for an explicit linearity threshold. The revised manuscript now contains an order-of-magnitude estimate, placed in the discussion of the secondary burst, for the scalar energy density at which the sourced metric perturbations would reach the scale of the background shell energy. Using the numerically obtained scalar amplitude and the resulting axial gravitational-wave energy, we show that the delayed secondary burst occurs at densities well below this threshold for the ultraweak couplings considered. This estimate supports the persistence of the linear regime throughout the reported evolution. revision: yes

Circularity Check

0 steps flagged

No circularity: results from direct numerical evolution of dCS perturbation equations

full rationale

The paper derives its claims via numerical integration of the linearized perturbation equations for the dCS pseudoscalar and axial gravitational modes in the presence of a fixed oscillating shell background. The Mathieu instability, Floquet sidebands, and secondary GW burst are outputs of that evolution; no parameter is fitted to data and then relabeled as a prediction, no self-citation supplies a load-bearing uniqueness theorem, and no ansatz is smuggled in. The derivation chain is therefore self-contained against the stated equations of motion.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

Based on the abstract only, the central claim rests on the effective field theory framework of dCS gravity, the modeling choice of an external oscillating shell, and the assumption that linear perturbations suffice to capture the instability and cascading effect. No new entities beyond the standard dCS pseudoscalar are introduced.

free parameters (2)
  • driving frequency of external shell
    Optimal value is stated to be set by resonant cavity length; specific values are chosen for numerical demonstrations.
  • dCS coupling strength
    Considered in the ultraweak regime; exact value not specified but treated as a tunable parameter for the instability to occur.
axioms (2)
  • domain assumption The effective field theory framework of dynamical Chern-Simons gravity is valid at the scales and couplings considered.
    The investigation is conducted entirely within this framework as stated in the abstract.
  • domain assumption Linear perturbation theory applies and backreaction from the amplified scalar field remains negligible during the instability growth.
    The mechanism of scalar amplification sourcing gravitational perturbations assumes the linear regime holds.

pith-pipeline@v0.9.1-grok · 5713 in / 1664 out tokens · 39507 ms · 2026-06-28T21:34:46.358280+00:00 · methodology

discussion (0)

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

Reference graph

Works this paper leans on

86 extracted references · 84 canonical work pages · 44 internal anchors

  1. [1]

    B. P. Abbottet al.(LIGO Scientific, Virgo), Phys. Rev. X6, 041015 (2016), [Erratum: Phys.Rev.X 8, 039903 (2018)], arXiv:1606.04856 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  2. [2]

    Constraining alternative theories of gravity using GW$150914$ and GW$151226$

    M. De Laurentis, O. Porth, L. Bovard, B. Ahmedov, and A. Abdujabbarov, Phys. Rev. D94, 124038 (2016), arXiv:1611.05766 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  3. [3]

    B. P. Abbottet al.(LIGO Scientific, Virgo), Phys. Rev. D100, 104036 (2019), arXiv:1903.04467 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  4. [4]

    B. P. Abbottet al.(LIGO Scientific, Virgo), Astrophys. J. Lett.892, L3 (2020), arXiv:2001.01761 [astro-ph.HE]

    work page arXiv 2020

  5. [5]

    Tests of General Relativity with GWTC-3

    R. Abbottet al.(LIGO Scientific, VIRGO, KAGRA), Phys. Rev. D112, 084080 (2025), arXiv:2112.06861 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  6. [6]

    A. K. Mehta, A. Buonanno, R. Cotesta, A. Ghosh, N. Sennett, and J. Steinhoff, Phys. Rev. D107, 044020 (2023), arXiv:2203.13937 [gr-qc]

    work page arXiv 2023

  7. [7]

    Payne, M

    E. Payne, M. Isi, K. Chatziioannou, L. Lehner, Y. Chen, and W. M. Farr, Phys. Rev. Lett.133, 251401 (2024), arXiv:2407.07043 [gr-qc]

    work page arXiv 2024

  8. [8]

    A. G. Abacet al.(LIGO Scientific, Virgo, KAGRA), Phys. Rev. Lett.136, 041403 (2026), arXiv:2509.08099 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  9. [9]

    C. M. Will, Living Rev. Rel.4, 4 (2001), arXiv:gr-qc/0103036

    work page internal anchor Pith review Pith/arXiv arXiv 2001

  10. [10]

    Bertotti, L

    B. Bertotti, L. Iess, and P. Tortora, Nature425, 374 (2003)

    2003

  11. [11]

    C. M. Will, Living Rev. Rel.17, 4 (2014), arXiv:1403.7377 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  12. [12]

    Testing general relativity using gravitational wave signals from the inspiral, merger and ringdown of binary black holes

    A. Ghosh, N. K. Johnson-Mcdaniel, A. Ghosh, C. K. Mishra, P. Ajith, W. Del Pozzo, C. P. L. Berry, A. B. Nielsen, and L. London, Class. Quant. Grav.35, 014002 (2018), arXiv:1704.06784 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  13. [13]

    Tests of General Relativity with Binary Black Holes from the second LIGO-Virgo Gravitational-Wave Transient Catalog

    R. Abbottet al.(LIGO Scientific, Virgo), Phys. Rev. D103, 122002 (2021), arXiv:2010.14529 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2021

  14. [14]

    N. V. Krishnendu and F. Ohme, Universe7, 497 (2021), arXiv:2201.05418 [gr-qc]

    work page arXiv 2021

  15. [15]

    Yang and C

    H. Yang and C. Lan, (2026), arXiv:2603.20594 [gr-qc]

    work page arXiv 2026

  16. [16]

    B. P. Abbottet al.(LIGO Scientific, Virgo), Phys. Rev. Lett.116, 221101 (2016), [Erratum: Phys.Rev.Lett. 121, 129902 (2018)], arXiv:1602.03841 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  17. [17]

    A. G. Abacet al.(LIGO Scientific, VIRGO, KAGRA), (2026), arXiv:2603.19019 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  18. [18]

    A. G. Abacet al.(LIGO Scientific, VIRGO, KAGRA), (2026), arXiv:2603.19020 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  19. [19]

    A. G. Abacet al.(LIGO Scientific, VIRGO, KAGRA), (2026), arXiv:2603.19021 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  20. [20]

    The US Program in Ground-Based Gravitational Wave Science: Contribution from the LIGO Laboratory

    D. Reitzeet al., Bull. Am. Astron. Soc.51, 141 (2019), arXiv:1903.04615 [astro-ph.IM]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  21. [21]

    Chern-Simons Modification of General Relativity

    R. Jackiw and S. Y. Pi, Phys. Rev. D68, 104012 (2003), arXiv:gr-qc/0308071

    work page internal anchor Pith review Pith/arXiv arXiv 2003

  22. [22]

    A gravitational-wave probe of effective quantum gravity

    S. Alexander, L. S. Finn, and N. Yunes, Phys. Rev. D78, 066005 (2008), arXiv:0712.2542 [gr-qc] . 27

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  23. [23]

    Dynamical Chern-Simons Modified Gravity I: Spinning Black Holes in the Slow-Rotation Approximation

    N. Yunes and F. Pretorius, Phys. Rev. D79, 084043 (2009), arXiv:0902.4669 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  24. [24]

    The Initial Value Formulation of Dynamical Chern-Simons Gravity

    T. Delsate, D. Hilditch, and H. Witek, Phys. Rev. D91, 024027 (2015), arXiv:1407.6727 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  25. [25]

    K. Yagi, N. Yunes, and T. Tanaka, Phys. Rev. Lett.109, 251105 (2012), [Erratum: Phys.Rev.Lett. 116, 169902 (2016), Erratum: Phys.Rev.Lett. 124, 029901 (2020)], arXiv:1208.5102 [gr-qc]

    work page arXiv 2012

  26. [26]

    Chern-Simons Modified General Relativity

    S. Alexander and N. Yunes, Phys. Rept.480, 1 (2009), arXiv:0907.2562 [hep-th]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  27. [27]

    Gravitational signature of Schwarzschild black holes in dynamical Chern-Simons gravity

    C. Molina, P. Pani, V. Cardoso, and L. Gualtieri, Phys. Rev. D81, 124021 (2010), arXiv:1004.4007 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  28. [28]

    H.-W. Hu, C. Lan, and Z.-K. Guo, (2025), arXiv:2511.21786 [gr-qc]

    work page arXiv 2025

  29. [29]

    Double Binary Pulsar Test of Dynamical Chern-Simons Modified Gravity

    N. Yunes and D. N. Spergel, Phys. Rev. D80, 042004 (2009), arXiv:0810.5541 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  30. [30]

    Gravitational Wave Tests of General Relativity with Ground-Based Detectors and Pulsar Timing Arrays

    N. Yunes and X. Siemens, Living Rev. Rel.16, 9 (2013), arXiv:1304.3473 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  31. [31]

    Extreme Gravity Tests with Gravitational Waves from Compact Binary Coalescences: (II) Ringdown

    E. Berti, K. Yagi, H. Yang, and N. Yunes, Gen. Rel. Grav.50, 49 (2018), arXiv:1801.03587 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  32. [32]

    R. Nair, S. Perkins, H. O. Silva, and N. Yunes, Phys. Rev. Lett.123, 191101 (2019), arXiv:1905.00870 [gr-qc]

    work page arXiv 2019

  33. [33]

    S. E. Perkins, R. Nair, H. O. Silva, and N. Yunes, Phys. Rev. D104, 024060 (2021), arXiv:2104.11189 [gr-qc]

    work page arXiv 2021

  34. [34]

    X. Che, X. Lyu, and C. Shi, (2025), arXiv:2512.22762 [gr-qc]

    work page arXiv 2025

  35. [35]

    Perturbations of Schwarzschild black holes in Dynamical Chern-Simons modified gravity

    V. Cardoso and L. Gualtieri, Phys. Rev. D80, 064008 (2009), [Erratum: Phys.Rev.D 81, 089903 (2010)], arXiv:0907.5008 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  36. [36]

    Evolving Metric Perturbations in dynamical Chern-Simons Gravity

    M. Okounkova, M. A. Scheel, and S. A. Teukolsky, Phys. Rev. D99, 044019 (2019), arXiv:1811.10713 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  37. [37]

    Wagle, N

    P. Wagle, N. Yunes, and H. O. Silva, Phys. Rev. D105, 124003 (2022), arXiv:2103.09913 [gr-qc]

    work page arXiv 2022

  38. [38]

    P. T. Leung, Y. T. Liu, W. M. Suen, C. Y. Tam, and K. Young, Phys. Rev. Lett.78, 2894 (1997), arXiv:gr-qc/9903031

    work page internal anchor Pith review Pith/arXiv arXiv 1997

  39. [39]

    A. J. M. Medved, D. Martin, and M. Visser, Class. Quant. Grav.21, 2393 (2004), arXiv:gr-qc/0310097

    work page internal anchor Pith review Pith/arXiv arXiv 2004

  40. [40]

    Can environmental effects spoil precision gravitational-wave astrophysics?

    E. Barausse, V. Cardoso, and P. Pani, Phys. Rev. D89, 104059 (2014), arXiv:1404.7149 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  41. [41]

    Bamber, O

    J. Bamber, O. J. Tattersall, K. Clough, and P. G. Ferreira, Phys. Rev. D103, 124013 (2021), arXiv:2103.00026 [gr-qc]

    work page arXiv 2021

  42. [42]

    Y. I. Maimon, A. B. Nielsen, and O. Birnholtz, Class. Quant. Grav.42, 185011 (2025), arXiv:2505.10199 [gr-qc]

    work page arXiv 2025

  43. [43]

    R. A. Konoplya and T. D. Pappas, JCAP02, 038 (2026), arXiv:2507.01954 [gr-qc]

    work page arXiv 2026

  44. [44]

    Lan, Y.-L

    C. Lan, Y.-L. Tian, H. Yang, Z.-X. Zhang, and Y.-G. Miao, Nucl. Phys. B1022, 117264 (2026), arXiv:2507.21414 [gr-qc]

    work page arXiv 2026

  45. [45]

    Akiyamaet al.(Event Horizon Telescope), Astrophys

    K. Akiyamaet al.(Event Horizon Telescope), Astrophys. J. Lett.910, L12 (2021), arXiv:2105.01169 [astro-ph.HE]

    work page arXiv 2021

  46. [46]

    Dark matter annihilation at the galactic center

    P. Gondolo and J. Silk, Phys. Rev. Lett.83, 1719 (1999), arXiv:astro-ph/9906391

    work page internal anchor Pith review Pith/arXiv arXiv 1999

  47. [47]

    C. F. B. Macedo, J. L. Rosa, and D. Rubiera-Garcia, JCAP07, 046 (2024), arXiv:2402.13047 [gr-qc]

    work page arXiv 2024

  48. [48]

    Kazempour, S

    S. Kazempour, S. Sun, and C. Yu, Phys. Rev. D110, 043034 (2024), arXiv:2404.11333 [hep-ph]

    work page arXiv 2024

  49. [49]

    Ranjbar and H

    R. Ranjbar and H. R. Olivares-S´ anchez, Astron. Astrophys.701, A27 (2025), arXiv:2502.12072 [astro-ph.HE]

    work page arXiv 2025

  50. [50]

    Y.-L. Tian, H. Yang, C. Lan, and Y.-G. Miao, Sci. China Phys. Mech. Astron.69, 230413 (2025), arXiv:2508.21381 [gr-qc]

    work page arXiv 2025

  51. [51]

    G. M. Tomaselli, T. F. M. Spieksma, and G. Bertone, JCAP07, 070 (2023), arXiv:2305.15460 [gr-qc]

    work page arXiv 2023

  52. [52]

    Mitra, S

    S. Mitra, S. Chakraborty, R. Vicente, and J. C. Feng, Phys. Rev. D110, 084012 (2024), arXiv:2312.06783 [gr-qc]

    work page arXiv 2024

  53. [53]

    Caneva Santoro, S

    G. Caneva Santoro, S. Roy, R. Vicente, M. Haney, O. J. Piccinni, W. Del Pozzo, and M. Martinez, Phys. Rev. Lett.132, 251401 (2024), arXiv:2309.05061 [gr-qc]

    work page arXiv 2024

  54. [54]

    M. H.-Y. Cheung, K. Destounis, R. P. Macedo, E. Berti, and V. Cardoso, Phys. Rev. Lett.128, 111103 (2022), arXiv:2111.05415 [gr-qc]

    work page arXiv 2022

  55. [55]

    R. A. Konoplya, A. F. Zinhailo, J. Kunz, Z. Stuchlik, and A. Zhidenko, JCAP10, 091 (2022), arXiv:2206.14714 [gr-qc]

    work page arXiv 2022

  56. [56]

    Cardoso, S

    V. Cardoso, S. Kastha, and R. Panosso Macedo, Phys. Rev. D110, 024016 (2024), arXiv:2404.01374 [gr-qc]

    work page arXiv 2024

  57. [57]

    P. H. C. Siqueira, L. T. de Paula, R. Panosso Macedo, and M. Richartz, Phys. Rev. D111, 104039 (2025), arXiv:2501.13815 [gr-qc]

    work page arXiv 2025

  58. [58]

    Oshita, E

    N. Oshita, E. Berti, and V. Cardoso, Phys. Rev. Lett.135, 031401 (2025), arXiv:2503.21276 [gr-qc]

    work page arXiv 2025

  59. [59]

    Black hole spectroscopy: from theory to experiment

    J. Abediet al., (2025), arXiv:2505.23895 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  60. [60]

    Hu, C.-J

    H.-W. Hu, C.-J. Fang, and Z.-K. Guo, (2025), arXiv:2512.11917 [gr-qc]

    work page arXiv 2025

  61. [61]

    Fujita, I

    T. Fujita, I. Obata, T. Tanaka, and K. Yamada, Class. Quant. Grav.38, 045010 (2021), arXiv:2008.02764 [gr-qc]

    work page arXiv 2021

  62. [62]

    M. P. G. Robbins, N. Afshordi, A. O. Jamison, and R. B. Mann, Class. Quant. Grav.39, 175009 (2022), arXiv:2101.03691 [gr-qc]

    work page arXiv 2022

  63. [63]

    L.-Y. Chen, H. Yu, and P. Wu, Phys. Lett. B849, 138457 (2024), arXiv:2401.07523 [gr-qc]

    work page arXiv 2024

  64. [64]

    Kehagias and A

    A. Kehagias and A. Riotto, (2025), arXiv:2512.05003 [gr-qc]

    work page arXiv 2025

  65. [65]

    G. R. Dvali, (1995), arXiv:hep-ph/9505253

    work page internal anchor Pith review Pith/arXiv arXiv 1995

  66. [66]

    Axions In String Theory

    P. Svrcek and E. Witten, JHEP06, 051 (2006), arXiv:hep-th/0605206

    work page internal anchor Pith review Pith/arXiv arXiv 2006

  67. [67]

    D. J. E. Marsh, Phys. Rept.643, 1 (2016), arXiv:1510.07633 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  68. [68]

    C. P. Burgess, G. Choi, and F. Quevedo, JHEP03, 051 (2024), arXiv:2301.00549 [hep-th]

    work page arXiv 2024

  69. [69]

    Alexander, H

    S. Alexander, H. Bernardo, and C. Creque-Sarbinowski, Phys. Rev. D110, 025015 (2024), arXiv:2403.15657 [hep-th]

    work page arXiv 2024

  70. [70]

    Alexander, G

    S. Alexander, G. Gabadadze, L. Jenks, and N. Yunes, (2025), arXiv:2512.00154 [hep-ph]

    work page arXiv 2025

  71. [71]

    H. O. Silva, J. Sakstein, L. Gualtieri, T. P. Sotiriou, and E. Berti, Phys. Rev. Lett.120, 131104 (2018), arXiv:1711.02080 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  72. [72]

    C. A. R. Herdeiro, E. Radu, N. Sanchis-Gual, and J. A. Font, Phys. Rev. Lett.121, 101102 (2018), arXiv:1806.05190 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  73. [73]

    Are black holes a serious threat to scalar field dark matter models?

    J. Barranco, A. Bernal, J. C. Degollado, A. Diez-Tejedor, M. Megevand, M. Alcubierre, D. Nunez, and O. Sarbach, Phys. Rev. D84, 083008 (2011), arXiv:1108.0931 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  74. [74]

    Schwarzschild black holes can wear scalar wigs

    J. Barranco, A. Bernal, J. C. Degollado, A. Diez-Tejedor, M. Megevand, M. Alcubierre, D. Nunez, and O. Sarbach, Phys. Rev. Lett.109, 081102 (2012), arXiv:1207.2153 [gr-qc] . 28

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  75. [75]

    B. Wang, C. Molina, and E. Abdalla, Phys. Rev. D63, 084001 (2001), arXiv:hep-th/0005143

    work page internal anchor Pith review Pith/arXiv arXiv 2001

  76. [76]

    Quasinormal behavior of massless scalar field perturbation in Reissner-Nordstrom anti-de Sitter spacetimes

    B. Wang, C.-Y. Lin, and C. Molina, Phys. Rev. D70, 064025 (2004), arXiv:hep-th/0407024

    work page internal anchor Pith review Pith/arXiv arXiv 2004

  77. [77]

    Boudet, F

    S. Boudet, F. Bombacigno, G. J. Olmo, and P. J. Porfirio, JCAP05, 032 (2022), arXiv:2203.04000 [gr-qc]

    work page arXiv 2022

  78. [78]

    Late-Time Behavior of Stellar Collapse and Explosions: I. Linearized Perturbations

    C. Gundlach, R. H. Price, and J. Pullin, Phys. Rev. D49, 883 (1994), arXiv:gr-qc/9307009

    work page internal anchor Pith review Pith/arXiv arXiv 1994

  79. [79]

    Peng, Z.-M

    Z.-Z. Peng, Z.-M. Zeng, C. Fu, and Z.-K. Guo, Phys. Rev. D106, 124044 (2022), arXiv:2209.10374 [gr-qc]

    work page arXiv 2022

  80. [80]

    W. H. Press and S. A. Teukolsky, Nature238, 211 (1972)

    1972

Showing first 80 references.