Pith. sign in

REVIEW 2 major objections 4 minor 2 cited by

A heavy axion's coherent oscillations can flip the sign of a light axion's effective potential, a Kapitza-type effect that the paper shows can boost the light axion's dark-matter abundance by two to three orders of magnitude.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

T0 review · deepseek-v4-flash

2026-08-04 17:11 UTC pith:VFFPU3LM

load-bearing objection The Kapitza sign-flip mechanism is real and well verified; the cosmological abundance enhancement is plausible but rests on the θosc ~ π heuristic. the 2 major comments →

arxiv 2509.11032 v1 pith:VFFPU3LM submitted 2025-09-14 hep-ph astro-ph.CO

Sign-Flipping Axion Potentials via Kapitza-Type Modulation by Heavy Axions

Kai Murai , Fuminobu Takahashi , Kosei Tomiyama This is my paper
classification hep-ph astro-ph.CO PACS 14.80.Va95.35.+d
keywords axionaxiverseKapitza pendulumsign flipBessel functiondark mattermisalignment mechanismtime averaging
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

This paper claims that a light axion's potential is not fixed by its own mass: when a heavier axion with which it mixes oscillates coherently with large amplitude, the time-averaged potential gains a multiplicative Bessel-function factor J0(A). Because J0(A) can be negative, the potential flips sign, so the point that was the minimum becomes the maximum and vice versa. The authors argue this 'Kapitza-type modulation' arises naturally from the mass hierarchy and mixing in the axiverse, requires no external drive, and can boost the light axion's dark-matter abundance by two to three orders of magnitude when the flip happens late in the radiation era. They demonstrate the effect numerically with the two-axion equations of motion and check where the time-averaged description breaks down.

Core claim

The central discovery is that the effective low-energy potential for a light axion χ, obtained by averaging over the fast oscillations of a heavy axion φ with mixing amplitude A = NΦ/fφ, is Veff(χ̄) = mχ² fχ² J0(A)(1 − cos(χ̄/fχ)). The Bessel function J0(A) controls both the height and the sign: for A ≳ 2.4, J0(A) < 0 and the stable and unstable field points interchange, so the light axion oscillates around the would-be maximum. When J0(A) crosses zero, the potential temporarily vanishes and the field can drift freely before the potential reappears. In an expanding universe the heavy axion's amplitude redshifts, so the sign flips multiple times if the mixing parameter N is large, and the fin

What carries the argument

The key object is the Bessel function J0(A) that emerges from time-averaging the cosine of a cosine, J0(A) = (mφ/2π)∫ dt cos[A cos(mφ t + α)]. It multiplies the entire effective potential, so its zeros at A ≈ 2.4, 5.5, 8.7, … turn the potential off entirely and its negative intervals flip the sign. The mass hierarchy Rm = mχ/mφ ≲ 0.01 makes the averaging valid, and the condition that the heavy-axion backreaction be negligible keeps the heavy field an external oscillator.

Load-bearing premise

The entire calculation assumes the time average over the heavy axion's oscillation is a valid description of the light axion's motion, which requires the mass ratio Rm to be small (≲0.01) and the light axion to start away from the hilltop; the paper itself shows both conditions can fail.

What would settle it

Simulate the full coupled equations with Rm = 0.4 and any initial phase α; the light axion's trajectory should visibly deviate from the time-averaged prediction (the paper's Fig. 4). For a crisp test of the sign flip itself, set Rm = 0.01, A = 3, and start θχ = 1; if the light axion does not settle around θχ = π while the heavy oscillation continues, the Bessel sign flip is wrong.

Watch this falsifier. Get emailed when new claim-graph text bears on it.

Share X Bluesky LinkedIn Reddit HN

If this is right

  • If J0(A) < 0 at late times, the light axion oscillates around a false vacuum; when J0(A) later becomes positive it must settle toward a true vacuum, delaying the onset of oscillations and enhancing the cold-axion abundance.
  • For large initial A, the abundance is enhanced by a factor (Ain/2.4)^{2/3} with a prefactor θosc² that can be as large as π², giving a total two-to-three order-of-magnitude enhancement over standard misalignment (Fig. 9).
  • The time-averaged description fails for Rm = O(0.1) and for hilltop initial conditions; in the latter case residual fast oscillations can carry the field across potential barriers (Fig. 5), which the effective potential alone would forbid.
  • The QCD axion can benefit: the Kapitza-induced false minimum is CP-conserving, so the trapped-misalignment-like delay occurs without the 10^{-3} fine-tuning of an explicit CP-violating term.
  • Perturbations of the light axion can grow via tachyonic instability with rate µk ∼ 2 sqrt[mχ² |J0(A)| cos θχ − k²] when Rm ≳ k/(sqrt(|J0|) mφ), potentially seeding structure or isocurvature.

Where Pith is reading between the lines

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

  • Nested hierarchies: in a clockwork chain of many axions, each heavier level would imprint its own J0 factor on the next, so a long ladder could produce repeated sign flips and quasi-free drifting epochs; the paper notes the idea but doesn't work it out.
  • The near-hilltop failure mode (Fig. 5) implies that the final vacuum number n is not determined by the averaged potential alone when initial conditions are close to a maximum; this introduces a phase-dependent, effectively stochastic element that could be a new source of axion isocurvature.
  • The mechanism is not exclusive to axions: any scalar with a mixing potential that is periodic in the heavy field, plus a mass hierarchy, should exhibit the same Bessel sign flip; this could be tested in condensed-matter systems with Floquet drives or in lattice simulations of two coupled scalars.
  • Since the heavy axion must dominate the energy density while the Kapitza effect acts (condition (41)), the model generically predicts a two-component dark matter sector; observations of the light axion's abundance alone would underestimate the total dark matter.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 4 minor

Summary. The paper considers a two-axion system with a large mass hierarchy and a periodic mixing potential. It shows that, after time-averaging over the rapid coherent oscillations of the heavy axion φ, the light axion χ experiences an effective potential Veff = mχ² fχ² J0(A) (1 − cos(χ/fχ)), where A = NΦ/fφ is the dimensionless heavy-axion amplitude. Since J0(A) can be negative, the sign of the light-axion potential flips, exchanging stable and unstable points; for A ≳ 2.4 the origin becomes unstable. The authors verify this Kapitza-type effect against the original equation of motion and identify the regimes where the effective description fails (insufficient mass hierarchy, hilltop initial conditions). They then analyze perturbation growth via parametric and tachyonic instabilities, and apply the sign-flip mechanism to axion dark matter. A late-time sign flip, caused by the redshift decay of A, is claimed to enhance the light-axion abundance by two to three orders of magnitude, with numerical support in Fig. 9.

Significance. If correct, this is a novel and elegant mechanism in multi-axion dynamics. The central derivation is simple and parameter-free, and the paper provides direct numerical verification of the original equations of motion (Figs. 2 and 3), not just the averaged equations. The explicit mapping of the breakdown of the effective description (Sec. II.D) is a particular strength and shows the authors' careful treatment of the approximation's limits. The perturbation analysis adds value, and the proposed cosmological application is plausible, though the quantitative abundance estimate is heuristic. The paper is likely to be of broad interest to the axion and dark-matter communities.

major comments (2)
  1. [Sec. IV.A, Eq. (40)] The paper's main cosmological payoff is the claimed two-to-three order enhancement of the light-axion abundance. This quantitative claim relies on the heuristic θosc≃π for Ain>2.4, introduced without derivation. The numerical results in Fig. 9 show sharp spikes where the enhancement is much larger and also regions where it is smaller, indicating a strong dependence on Ain and on whether the field lands near a hilltop. To support the claim that the enhancement is generic, the authors should either justify θosc more systematically or scan over initial field values and the phase α. As written, the quantitative enhancement is an order-of-magnitude estimate rather than a robust prediction.
  2. [Sec. IV.A] The abundance calculation assumes a radiation-dominated universe with H=1/(2t) and a(t)∝t^{1/2}. However, the backreaction discussion leading to Eq. (42) shows that the heavy axion energy density can exceed that of the light axion by a large factor for Ain≫1; it does not ensure ρφ is subdominant to radiation at the times of interest. If ρφ dominates, the expansion history and the amplitude-redshift law A∝a^{-3/2} used in Eq. (31) would be modified, affecting the estimate of tosc and the abundance (40). The paper should either impose the additional constraint ρφ(t)<ρrad(t) for the benchmark parameters or state clearly the regime where the radiation-dominated approximation is valid.
minor comments (4)
  1. [Sec. IV.A/Fig. 9] Please state explicitly whether the numerical results in Fig. 9 are obtained by solving the original time-dependent equation (with the full oscillating source and Hubble expansion) or the time-averaged effective equation. This is important because the validity of the effective description across multiple sign flips is a key concern for large Ain.
  2. [Sec. IV.A, Eqs. (34)-(35)] The definition of tosc is ambiguous. Equation (34) uses A(tosc)≈2.4, the zero of J0, while the text says A(tosc) is smaller than the first zero and the onset is set by 3H=meff. Clarify that tosc is approximately the last sign-flip time in the limit meff≪mχ, or revise the formulas to distinguish the flip time from the oscillation-onset time.
  3. [Eq. (42)] The typography of Eq. (42) is difficult to follow; the placement of the denominator factors (Ain/2.4)^(-4/3) is not immediately clear. Please rewrite with explicit fractions for readability.
  4. [Sec. III.A] The parametric-resonance result in Fig. 6 is obtained for Rm∼O(0.1), which is outside the regime where the time-averaged description is used for the abundance calculation. It would help to state explicitly that this channel is subdominant in the benchmark regime and is included for completeness.

Circularity Check

0 steps flagged

No significant circularity: the Kapitza-type effective potential is a parameter-free time average, verified against the original equations of motion, and the cosmological abundance is computed from given inputs rather than fitted.

full rationale

The paper's central claim is the derivation of Veff from Eq. (2): substituting the heavy-axion solution ϕ=Φ cos(mϕt+α) into Vmix and averaging over one fast period gives Veff=mχ² fχ² J0(A)(1−cos(χ̄/fχ)) (Eqs. (11)–(14)). This is a mathematical identity, not a definition of χ̄ in terms of Veff, and the coefficient J0(A) is obtained by known integrals, not by fitting. The paper then validates the time-averaged description against numerical solutions of the original nonlinear equation (9) (Fig. 2) and explicitly identifies where it fails: insufficient mass hierarchy (Sec. II.D.1, Rm=0.4) and hilltop initial conditions (Sec. II.D.2, |θχ(0)|≪1). These are disclosed limitations rather than concealed circularity. The cosmological abundance (Eqs. (39)–(40)) is computed from the specified input parameters (mχ, fχ, Ain) using both an analytic estimate with an explicit ansatz θ_osc∼π and numerical integration of the original equations; the analytic estimate is labeled rough ('a crude estimate') and is compared to, not used to fit, the red dots in Fig. 9. No parameter is fitted to the target abundance, and the enhancement appears as an output. Self-citations appear for auxiliary mechanisms (clockwork, trapped/bubble misalignment) used only to motivate large Ain, but these are not invoked as proof of the sign-flip or as a uniqueness theorem, and they are accompanied by independent references. The paper contains no self-definitional step, no fitted input renamed as prediction, and no load-bearing self-citation chain.

Axiom & Free-Parameter Ledger

1 free parameters · 6 axioms · 0 invented entities

The paper uses a two-axion mixing model with hierarchical masses, a standard setup in axiverse phenomenology. No new particles or forces are introduced. The central claim depends on the validity of time averaging and the stated hierarchy conditions; the abundance result further depends on the assumed decay of the heavy axion amplitude and on the heuristic θosc ≈ π.

free parameters (1)
  • θosc (oscillation amplitude of light axion at tosc) = π (assumed for Ain > 2.4; order 1 for Ain < 2.4)
    Used in Eqs. (36)-(40) for the abundance estimate; the value is justified only heuristically by the expected large displacement during the sign flip and is not derived from first principles.
axioms (6)
  • domain assumption The two-axion potential is given by Eqs. (1)-(2) with hierarchical masses mφ ≫ mχ.
    The entire analysis is based on this specific Lagrangian; the axiverse is cited as motivation for such a hierarchy.
  • domain assumption The heavy axion φ can be treated as a homogeneous external field with negligible backreaction from χ, Eq. (4).
    Needed to replace φ(t) by Eq. (7) and to neglect ∂Vmix/∂φ in the heavy axion equation of motion; the paper notes this condition must hold until tosc for the cosmological application.
  • domain assumption The time-averaging procedure replacing cos[A cos(mφt) + ...] with J0(A) is valid, i.e., the dynamics of χ are slow compared to φ oscillations.
    The central approximation behind Eq. (14); the paper itself shows it fails for Rm = 0.4 and near hilltop initial conditions.
  • domain assumption In the expanding universe, the heavy axion amplitude decays as a^(-3/2) in a quadratic potential, Eq. (31).
    Used to derive the time dependence of A(t) and the timing of the final sign flip tosc in Sec. IV.
  • domain assumption The clockwork mechanism or trapped/bubble misalignment can provide N ≫ 1 or delayed onset, respectively, to make Ain large.
    Required for the cosmological scenario where J0(A) crosses zero multiple times; not derived within this paper, only cited.
  • standard math Standard Bessel-function integral identities and Floquet theory for parametric resonance.
    The time averages in Eqs. (12)-(13) and the instability analysis in Sec. III use standard mathematical results.

pith-pipeline@v1.3.0-alltime-deepseek · 16018 in / 8383 out tokens · 103175 ms · 2026-08-04T17:11:41.116728+00:00 · methodology

0 comments
Cite this review

Pith. "Pith review of Sign-Flipping Axion Potentials via Kapitza-Type Modulation by Heavy Axions." pith.science (2026). https://pith.science/paper/VFFPU3LM

@misc{pith2026250911032,
  author       = {Pith},
  title        = {Pith review of: Sign-Flipping Axion Potentials via Kapitza-Type Modulation by Heavy Axions},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/VFFPU3LM}},
  note         = {Machine review of arXiv:2509.11032}
}
Share X Bluesky LinkedIn Reddit HN
read the original abstract

We show that the potential of a light axion can flip sign, or even nearly vanish, as a result of coherent oscillations of a heavier axion with which it mixes. This phenomenon is analogous to the Kapitza pendulum, where a high-frequency external force stabilizes an otherwise unstable configuration, but here it arises naturally from the inherent mass hierarchy and mixing among axions in the axiverse, without the need for any externally imposed modulation. We further show that a late-time sign flip of the potential can significantly enhance the abundance of the light axion, which has important cosmological and observational consequences.

Figures

Figures reproduced from arXiv: 2509.11032 by Fuminobu Takahashi, Kai Murai, Kosei Tomiyama.

Figure 1
Figure 1. Figure 1: FIG. 1 [PITH_FULL_IMAGE:figures/full_fig_p007_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2. Numerical solutions of the original (solid) and time-averaged (dashed) equations of motion [PITH_FULL_IMAGE:figures/full_fig_p008_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3. Time evolution of [PITH_FULL_IMAGE:figures/full_fig_p009_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4. Time evolution of [PITH_FULL_IMAGE:figures/full_fig_p011_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: shows that when α = 0, the behavior relatively follows the time-averaged case. This is because the residual fluctuations are minimal for α = 0. III. GROWTH OF PERTURBATIONS UNDER THE KAPITZA-TYPE MODU￾LATIONS In the previous section, we discussed the spatially homogeneous components of the two axions. In this section, we continue to treat the heavy axion ϕ as a spatially homogeneous 12 [PITH_FULL_IMAGE:fi… view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6. Numerical result for the growth rate with [PITH_FULL_IMAGE:figures/full_fig_p014_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: FIG. 7. The numerical result of the growth rate with [PITH_FULL_IMAGE:figures/full_fig_p016_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: FIG. 8. The growth rate of occupation number with [PITH_FULL_IMAGE:figures/full_fig_p017_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: FIG. 9. Axion abundance as a function of [PITH_FULL_IMAGE:figures/full_fig_p023_9.png] view at source ↗

discussion (0)

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

Forward citations

Cited by 2 Pith papers

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

  1. Hierarchical Axiverse

    hep-ph 2026-08 reject novelty 5.0

    The paper asserts that the requirement of well-defined QCD-induced mixing alone forces ALP masses into a hierarchical spacing and decay constants into two separated populations, but it does not demonstrate the underly...

  2. Stochastic Axion Mixing: A General Mechanism Beyond Decay Constant Constraints

    hep-ph 2026-04 unverdicted novelty 5.0

    Stochastic axion mixing is a broad mechanism for axion interactions in multi-axion systems that occurs naturally under distinct mass conditions and does not depend on decay constant hierarchies.

Reference graph

Works this paper leans on

85 extracted references · 66 linked inside Pith · cited by 2 Pith papers

  1. [1]

    Insufficient Mass Hierarchy First, we consider the case in which the mass hierarchy is insufficient. Fig. 4 shows the time evolution ofθ χ forR m = 0.4. In this case, the mass hierarchy between the two axions is not large enough, so the oscillation ofϕsignificantly affects the evolution of¯χ, and the use of the time-averaged equation is no longer valid. A...

  2. [2]

    In this case,¯χinitially evolves slowly with a tiny amplitude, similar to slow-roll behavior

    Hilltop Initial Conditions Next, we consider a situation in which¯χis initially located near the hilltop of the effective potential, e.g.,|¯χ(0)| ≪fχ whenJ 0(A)<0. In this case,¯χinitially evolves slowly with a tiny amplitude, similar to slow-roll behavior. Whenθχ is sufficiently small,θχ ≪1, Eq. (9) can be approximated as ¨¯χ+R2 mm2 ϕfχ [sin (Acos (mϕt+α...

  3. [3]

    R. D. Peccei and H. R. Quinn, Phys. Rev. Lett.38, 1440 (1977)

    1977

  4. [4]

    R. D. Peccei and H. R. Quinn, Phys. Rev. D16, 1791 (1977)

    1977

  5. [5]

    Weinberg, Phys

    S. Weinberg, Phys. Rev. Lett.40, 223 (1978)

    1978

  6. [6]

    Wilczek, Phys

    F. Wilczek, Phys. Rev. Lett.40, 279 (1978)

    1978

  7. [7]

    J. E. Kim and G. Carosi, Rev. Mod. Phys.82, 557 (2010), [Erratum: Rev.Mod.Phys. 91, 049902 (2019)], arXiv:0807.3125 [hep-ph]. 25

    Pith/arXiv arXiv 2010

  8. [8]

    Arias, D

    P. Arias, D. Cadamuro, M. Goodsell, J. Jaeckel, J. Redondo, and A. Ringwald, JCAP06, 013 (2012), arXiv:1201.5902 [hep-ph]

    Pith/arXiv arXiv 2012

  9. [9]

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

    Pith/arXiv arXiv 2016

  10. [10]

    Di Luzio, M

    L. Di Luzio, M. Giannotti, E. Nardi, and L. Visinelli, Phys. Rept.870, 1 (2020), arXiv:2003.01100 [hep-ph]

    Pith/arXiv arXiv 2020

  11. [11]

    C. A. J. O’Hare, PoSCOSMICWISPers, 040 (2024), arXiv:2403.17697 [hep-ph]

    Pith/arXiv arXiv 2024

  12. [12]

    Arvanitaki, S

    A. Arvanitaki, S. Dimopoulos, S. Dubovsky, N. Kaloper, and J. March-Russell, Phys. Rev. D 81, 123530 (2010), arXiv:0905.4720 [hep-th]

    Pith/arXiv arXiv 2010

  13. [13]

    Higaki and F

    T. Higaki and F. Takahashi, JHEP07, 074 (2014), arXiv:1404.6923 [hep-th]

    Pith/arXiv arXiv 2014

  14. [14]

    T.Higaki, K.S.Jeong, N.Kitajima, andF.Takahashi,JHEP06,150(2016),arXiv:1603.02090 [hep-ph]

    Pith/arXiv arXiv 2016

  15. [15]

    Farina, D

    M. Farina, D. Pappadopulo, F. Rompineve, and A. Tesi, JHEP01, 095 (2017), arXiv:1611.09855 [hep-ph]

    Pith/arXiv arXiv 2017

  16. [16]

    C. T. Hill and G. G. Ross, Nucl. Phys. B311, 253 (1988)

    1988

  17. [17]

    Kitajima and F

    N. Kitajima and F. Takahashi, JCAP01, 032 (2015), arXiv:1411.2011 [hep-ph]

    Pith/arXiv arXiv 2015

  18. [18]

    Daido, N

    R. Daido, N. Kitajima, and F. Takahashi, Phys. Rev. D92, 063512 (2015), arXiv:1505.07670 [hep-ph]

    Pith/arXiv arXiv 2015

  19. [19]

    Daido, N

    R. Daido, N. Kitajima, and F. Takahashi, Phys. Rev. D93, 075027 (2016), arXiv:1510.06675 [hep-ph]

    Pith/arXiv arXiv 2016

  20. [20]

    S.-Y. Ho, K. Saikawa, and F. Takahashi, JCAP10, 042 (2018), arXiv:1806.09551 [hep-ph]

    Pith/arXiv arXiv 2018

  21. [21]

    Murai, F

    K. Murai, F. Takahashi, and W. Yin, Phys. Rev. D108, 036020 (2023), arXiv:2305.18677 [hep-ph]

    Pith/arXiv arXiv 2023

  22. [22]

    Cyncynates and J

    D. Cyncynates and J. O. Thompson, Phys. Rev. D108, L091703 (2023), arXiv:2306.04678 [hep-ph]

    Pith/arXiv arXiv 2023

  23. [23]

    Li, JCAP09, 025 (2024), arXiv:2307.09245 [hep-ph]

    H.-J. Li, JCAP09, 025 (2024), arXiv:2307.09245 [hep-ph]

    Pith/arXiv arXiv 2024

  24. [24]

    Li, Y.-Q

    H.-J. Li, Y.-Q. Peng, W. Chao, and Y.-F. Zhou, Phys. Lett. B849, 138444 (2024), arXiv:2310.02126 [hep-ph]

    Pith/arXiv arXiv 2024

  25. [25]

    Li and Y.-F

    H.-J. Li and Y.-F. Zhou, (2024), arXiv:2401.09138 [hep-ph]

    Pith/arXiv arXiv 2024

  26. [26]

    Li and Y.-F

    H.-J. Li and Y.-F. Zhou, (2024), arXiv:2408.00267 [hep-ph]

    Pith/arXiv arXiv 2024

  27. [27]

    Murai, Y

    K. Murai, Y. Narita, F. Takahashi, and W. Yin, JHEP04, 124 (2025), arXiv:2412.10232 [hep-ph]. 26

    Pith/arXiv arXiv 2025

  28. [28]

    D. I. Dunsky, C. A. Manzari, P. Quílez, M. Ramos, and P. Sørensen, (2025), arXiv:2507.06287 [hep-ph]

    Pith/arXiv arXiv 2025

  29. [29]

    K. Choi, H. Kim, and S. Yun, Phys. Rev. D90, 023545 (2014), arXiv:1404.6209 [hep-th]

    Pith/arXiv arXiv 2014

  30. [30]

    Nakayama, F

    K. Nakayama, F. Takahashi, and T. T. Yanagida, JHEP09, 014 (2014), arXiv:1406.4265 [hep-ph]

    Pith/arXiv arXiv 2014

  31. [31]

    Daido, F

    R. Daido, F. Takahashi, and W. Yin, JCAP05, 044 (2017), arXiv:1702.03284 [hep-ph]

    Pith/arXiv arXiv 2017

  32. [32]

    Takahashi and W

    F. Takahashi and W. Yin, JHEP10, 120 (2019), arXiv:1908.06071 [hep-ph]

    Pith/arXiv arXiv 2019

  33. [33]

    Kobayashi and L

    T. Kobayashi and L. Ubaldi, JHEP08, 147 (2019), arXiv:1907.00984 [hep-ph]

    Pith/arXiv arXiv 2019

  34. [34]

    Kobayashi and L

    T. Kobayashi and L. Ubaldi, JHEP09, 052 (2020), arXiv:2006.09389 [hep-ph]

    Pith/arXiv arXiv 2020

  35. [35]

    Narita, F

    Y. Narita, F. Takahashi, and W. Yin, JCAP12, 039 (2023), arXiv:2308.12154 [hep-ph]

    Pith/arXiv arXiv 2023

  36. [36]

    Cyncynates, T

    D. Cyncynates, T. Giurgica-Tiron, O. Simon, and J. O. Thompson, Phys. Rev. D105, 055005 (2022), arXiv:2109.09755 [hep-ph]

    Pith/arXiv arXiv 2022

  37. [37]

    Higaki, N

    T. Higaki, N. Kitajima, and F. Takahashi, JCAP12, 004 (2014), arXiv:1408.3936 [hep-ph]

    Pith/arXiv arXiv 2014

  38. [38]

    Higaki, K

    T. Higaki, K. S. Jeong, N. Kitajima, T. Sekiguchi, and F. Takahashi, JHEP08, 044 (2016), arXiv:1606.05552 [hep-ph]

    Pith/arXiv arXiv 2016

  39. [39]

    A. J. Long, JHEP07, 066 (2018), arXiv:1803.07086 [hep-ph]

    Pith/arXiv arXiv 2018

  40. [40]

    M. Eto, T. Hiramatsu, I. Saito, and Y. Sakakihara, Phys. Rev. D108, 116004 (2023), arXiv:2309.04248 [hep-th]

    Pith/arXiv arXiv 2023

  41. [41]

    J. Lee, K. Murai, F. Takahashi, and W. Yin, JCAP10, 038 (2024), arXiv:2407.09478 [hep-ph]

    Pith/arXiv arXiv 2024

  42. [42]

    J. Lee, K. Murai, F. Takahashi, and W. Yin, JCAP04, 002 (2025), arXiv:2409.09749 [hep-ph]

    Pith/arXiv arXiv 2025

  43. [43]

    J. Lee, K. Murai, F. Takahashi, and W. Yin, (2025), arXiv:2507.07075 [hep-ph]

    arXiv 2025

  44. [44]

    Kondo and H

    D. Kondo and H. Murayama, (2025), arXiv:2507.07973 [hep-ph]

    arXiv 2025

  45. [45]

    Kobayashi, R

    T. Kobayashi, R. Kurematsu, and F. Takahashi, JCAP09, 032 (2013), arXiv:1304.0922 [hep- ph]

    Pith/arXiv arXiv 2013

  46. [46]

    I. L. Bogolyubsky and V. G. Makhankov, Pisma Zh. Eksp. Teor. Fiz.24, 15 (1976)

    1976

  47. [47]

    Gleiser, Phys

    M. Gleiser, Phys. Rev. D49, 2978 (1994), arXiv:hep-ph/9308279

    Pith/arXiv arXiv 1994

  48. [48]

    Kasuya, M

    S. Kasuya, M. Kawasaki, and F. Takahashi, Phys. Lett. B559, 99 (2003), arXiv:hep- ph/0209358

    arXiv 2003

  49. [49]

    Nakagawa, F

    S. Nakagawa, F. Takahashi, and M. Yamada, JCAP05, 062 (2021), arXiv:2012.13592 [hep-ph]

    Pith/arXiv arXiv 2021

  50. [50]

    Di Luzio, B

    L. Di Luzio, B. Gavela, P. Quilez, and A. Ringwald, JCAP10, 001 (2021), arXiv:2102.01082 [hep-ph]. 27

    Pith/arXiv arXiv 2021

  51. [51]

    K. S. Jeong, K. Matsukawa, S. Nakagawa, and F. Takahashi, JCAP03, 026 (2022), arXiv:2201.00681 [hep-ph]

    Pith/arXiv arXiv 2022

  52. [52]

    Di Luzio and P

    L. Di Luzio and P. Sørensen, JHEP10, 239 (2024), arXiv:2408.04623 [hep-ph]

    Pith/arXiv arXiv 2024

  53. [53]

    Nakagawa, F

    S. Nakagawa, F. Takahashi, M. Yamada, and W. Yin, Phys. Lett. B839, 137824 (2023), arXiv:2210.10022 [hep-ph]

    Pith/arXiv arXiv 2023

  54. [54]

    J. Lee, K. Murai, F. Takahashi, and W. Yin, JCAP05, 122 (2024), arXiv:2402.09501 [hep-ph]

    Pith/arXiv arXiv 2024

  55. [55]

    Hook and J

    A. Hook and J. Huang, JHEP06, 036 (2018), arXiv:1708.08464 [hep-ph]

    Pith/arXiv arXiv 2018

  56. [56]

    Balkin, J

    R. Balkin, J. Serra, K. Springmann, and A. Weiler, JHEP07, 221 (2020), arXiv:2003.04903 [hep-ph]

    Pith/arXiv arXiv 2020

  57. [57]

    Balkin, J

    R. Balkin, J. Serra, K. Springmann, S. Stelzl, and A. Weiler, JHEP02, 141 (2025), arXiv:2307.14418 [hep-ph]

    Pith/arXiv arXiv 2025

  58. [58]

    Kumamoto, J

    M. Kumamoto, J. Huang, C. Drischler, M. Baryakhtar, and S. Reddy, (2024), arXiv:2410.21590 [hep-ph]

    Pith/arXiv arXiv 2024

  59. [59]

    R. T. Co, E. Gonzalez, and K. Harigaya, JHEP05, 163 (2019), arXiv:1812.11192 [hep-ph]

    Pith/arXiv arXiv 2019

  60. [60]

    Takahashi and W

    F. Takahashi and W. Yin, JHEP07, 095 (2019), arXiv:1903.00462 [hep-ph]

    Pith/arXiv arXiv 2019

  61. [61]

    Nakagawa, F

    S. Nakagawa, F. Takahashi, and W. Yin, JCAP05, 004 (2020), arXiv:2002.12195 [hep-ph]

    Pith/arXiv arXiv 2020

  62. [62]

    Huang, A

    J. Huang, A. Madden, D. Racco, and M. Reig, JHEP10, 143 (2020), arXiv:2006.07379 [hep- ph]

    Pith/arXiv arXiv 2020

  63. [63]

    Gonzalez, N

    D. Gonzalez, N. Kitajima, F. Takahashi, and W. Yin, Phys. Lett. B843, 137990 (2023), arXiv:2211.06849 [hep-ph]

    Pith/arXiv arXiv 2023

  64. [64]

    R. T. Co, T. Gherghetta, Z. Liu, and K.-F. Lyu, JHEP09, 145 (2024), arXiv:2407.12930 [hep-ph]

    Pith/arXiv arXiv 2024

  65. [65]

    Khoury, M.-X

    J. Khoury, M.-X. Lin, and M. Trodden, (2025), arXiv:2503.16415 [astro-ph.CO]

    arXiv 2025

  66. [66]

    P. L. Kapitza, Soviet Physics JETP21, 588 (1951), english translation of Zh. Eksp. Teor. Fiz. 21, 588 (1951)

    1951

  67. [67]

    Stephenson, The London, Edinburgh, and Dublin Philosophical Magazine and Journal of Science 6,15, 233 (1908)

    A. Stephenson, The London, Edinburgh, and Dublin Philosophical Magazine and Journal of Science 6,15, 233 (1908)

    1908

  68. [68]

    Bukov, L

    M. Bukov, L. D’Alessio, and A. Polkovnikov, Advances in Physics64, 139 (2015), arXiv:1407.4803

    Pith/arXiv arXiv 2015

  69. [69]

    Choi and S

    K. Choi and S. H. Im, JHEP01, 149 (2016), arXiv:1511.00132 [hep-ph]

    Pith/arXiv arXiv 2016

  70. [70]

    D. E. Kaplan and R. Rattazzi, Phys. Rev. D93, 085007 (2016), arXiv:1511.01827 [hep-ph]. 28

    Pith/arXiv arXiv 2016

  71. [71]

    Higaki, K

    T. Higaki, K. S. Jeong, N. Kitajima, and F. Takahashi, Phys. Lett. B755, 13 (2016), arXiv:1512.05295 [hep-ph]

    Pith/arXiv arXiv 2016

  72. [72]

    K. S. Jeong, K. Matsukawa, S. Nakagawa, and F. Takahashi, Journal of Cosmology and Astroparticle Physics2022, 026 (2022)

    2022

  73. [73]

    A. G. Cohen and D. B. Kaplan, Phys. Lett. B199, 251 (1987)

    1987

  74. [74]

    A. G. Cohen and D. B. Kaplan, Nucl. Phys. B308, 913 (1988)

    1988

  75. [75]

    M. Dine, P. Huet, R. L. Singleton, Jr, and L. Susskind, Phys. Lett. B257, 351 (1991)

    1991

  76. [76]

    A. G. Cohen, D. B. Kaplan, and A. E. Nelson, Phys. Lett. B263, 86 (1991)

    1991

  77. [77]

    Dolgov and K

    A. Dolgov and K. Freese, Phys. Rev. D51, 2693 (1995), arXiv:hep-ph/9410346

    Pith/arXiv arXiv 1995

  78. [78]

    Dolgov, K

    A. Dolgov, K. Freese, R. Rangarajan, and M. Srednicki, Phys. Rev. D56, 6155 (1997), arXiv:hep-ph/9610405

    Pith/arXiv arXiv 1997

  79. [79]

    Chiba, F

    T. Chiba, F. Takahashi, and M. Yamaguchi, Phys. Rev. Lett.92, 011301 (2004), [Erratum: Phys.Rev.Lett. 114, 209901 (2015)], arXiv:hep-ph/0304102

    Pith/arXiv arXiv 2004

  80. [80]

    Takahashi and M

    F. Takahashi and M. Yamaguchi, Phys. Rev. D69, 083506 (2004), arXiv:hep-ph/0308173

    Pith/arXiv arXiv 2004

Showing first 80 references.