pith. sign in

arxiv: 2606.31430 · v1 · pith:YHEU4RMAnew · submitted 2026-06-30 · 🌌 astro-ph.CO

One Feature, Three Clocks: Phase-Locked Gravitational Waves, Primordial Black Holes, and Non-Gaussianity from Periodic Warm Inflation

Mayukh R. Gangopadhyay This is my paper

Pith reviewed 2026-07-01 04:24 UTC · model grok-4.3

classification 🌌 astro-ph.CO
keywords warm inflationperiodic couplingprimordial black holesscalar-induced gravitational wavesnon-Gaussianitylog-periodic modulationthermal frictionbispectrum phase
0
0 comments X

The pith

A periodic friction feature in warm inflation imprints the same log-periodic structure on two gravitational-wave bands, asteroid-mass primordial black holes, and a phase-shifted bispectrum.

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

The paper establishes that a shift-symmetric inflaton dissipating into a thermal bath with periodic coupling experiences a friction surge when the thermal channel opens midway through rolling. This surge leaves CMB scales untouched but creates a sharp log-periodically modulated peak in the curvature spectrum at small scales. The peak saturates PBH formation in the asteroid-mass window at an order-unity dark-matter fraction and sources scalar-induced gravitational waves in two bands that share the same log-period and freeze-out phase to leading order. A separate-universe computation shows the equilateral bispectrum offset by a quarter cycle from the power spectrum, an offset fixed by the running of the spectrum. A reader would care because the feature is localized in field space, so one underlying clock ties gravitational-wave bands, black-hole mass, and bispectrum phase together in a way a single-scale feature cannot reproduce.

Core claim

When the thermal channel opens midway, the periodic coupling causes friction to surge and imprint a log-periodically modulated peak on the curvature power spectrum at small scales. This peak saturates PBH formation in the asteroid-mass window and sources two bands of scalar-induced gravitational waves with matching log-period and freeze-out phase, while the equilateral bispectrum is offset by π/2 from the power spectrum due to the spectrum's running. The high-frequency band is itself bounded by PBH overproduction, which constrains how far friction can grow. The two GW bands and the bispectrum are expected to share the log-periodic structure because the feature is localized in the field.

What carries the argument

The periodic coupling of the inflaton to the thermal bath, which makes friction oscillate and surge when the channel opens at an intermediate field value, localizing the feature so it imprints the same log-periodic structure on multiple observables.

If this is right

  • The gravitational-wave spectrum shows a peak near 3 mHz for LISA and a second band from deci-hertz to a hundred hertz within reach of DECIGO and the Einstein Telescope, both carrying the same log-period and phase to leading order.
  • The high-frequency gravitational-wave band is bounded by PBH overproduction, which constrains how far the friction can grow.
  • The equilateral bispectrum shares the log-periodic structure with a phase offset fixed by the running of the spectrum and therefore robust to the equilateral-shape coefficient.
  • Primordial black holes in the asteroid-mass window can make up an order-unity fraction of the dark matter.

Where Pith is reading between the lines

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

  • Detection of matching modulations in the two widely separated GW bands would favor a single localized field feature over independent mechanisms at each scale.
  • The same periodic-coupling setup could be applied to other inflationary models to predict consistent multi-probe signatures at additional frequency windows.
  • A measured phase offset in the bispectrum that deviates from the quarter-cycle prediction would test the claim that the offset is fixed solely by spectrum running.

Load-bearing premise

The thermal channel opens at a specific intermediate field value chosen so the friction surge affects only small scales while leaving CMB scales untouched, together with the assumed functional form of the periodic coupling.

What would settle it

Detection or non-detection of gravitational waves in the two predicted bands that either match or fail to match in log-period and phase, or a measurement of the equilateral bispectrum showing or lacking the expected quarter-cycle offset relative to the power spectrum.

Figures

Figures reproduced from arXiv: 2606.31430 by Mayukh R. Gangopadhyay.

Figure 1
Figure 1. Figure 1: FIG. 1. No second resonant crossing re-saturates the spectrum. [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 3
Figure 3. Figure 3: shows the resulting spectrum, with the inset re￾solving the periodic feature against the smooth (δ = 0) case. Two independent checks confirm this, including the thermal noise: convolving the exact G(Q) through the freeze-out window, and evolving the overdamped warm [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4. Left: the freeze-out transfer function [PITH_FULL_IMAGE:figures/full_fig_p009_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5. Differential PBH abundance for the oscillatory (red) [PITH_FULL_IMAGE:figures/full_fig_p009_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6. Power-law-integrated sensitivity (PLS) curves [PITH_FULL_IMAGE:figures/full_fig_p011_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: FIG. 7. Left: the equilateral non-Gaussianity [PITH_FULL_IMAGE:figures/full_fig_p013_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: FIG. 8. The correlated signature: the three observables on [PITH_FULL_IMAGE:figures/full_fig_p013_8.png] view at source ↗
read the original abstract

A shift-symmetric inflaton dissipating into a thermal bath couples to that bath periodically, so its friction oscillates as the field rolls. We follow what this does to warm inflation when a thermal channel opens midway through the rolling: the friction surges, and the curvature spectrum grows a sharp, log-periodically modulated peak at small scales while the CMB scales stay untouched. It saturates Primordial Black Holes (PBHs) formation in the asteroid-mass window, where the PBHs can make up an order-unity fraction of the dark matter, and it sources a scalar-induced gravitational-wave background in two bands at once -- a peak at $h^2\Omega_{\rm GW}\simeq10^{-8}$ near $3$~mHz for LISA, and a second band at $h^2\Omega_{\rm GW}\sim10^{-11}$ from deci-hertz to a hundred hertz, within reach of DECIGO and the Einstein Telescope, fed by the friction's continued growth toward smaller scales. And a separate-universe computation places its equilateral bispectrum a quarter cycle ahead of the power spectrum -- an offset fixed by the running of the spectrum and so robust to the equilateral-shape coefficient. The two GW bands carry the same underlying log-period and freeze-out phase to leading order, and the bispectrum is expected to share them: a modulation seen at two widely separated frequencies, plausibly accompanied by a $\pi/2$-shifted bispectrum, is not something a single-scale feature can fake. Because the feature is localized in the field, it imprints the same log-periodic structure on multiple observables, tying the gravitational-wave bands, black-hole mass, and bispectrum phase to a single underlying clock. We derive the freeze-out transfer function in closed form and use it to cap the first two harmonics at one quarter, and we show that the high-frequency band is itself bounded by PBHs overproduction, which turns it into a constraint on how far the friction can grow.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The paper proposes a model of periodic warm inflation where a shift-symmetric inflaton couples periodically to a thermal bath. A thermal channel opens midway through the roll, surging friction and producing a sharp log-periodically modulated peak in the small-scale curvature spectrum (leaving CMB scales untouched). This saturates PBH formation in the asteroid-mass window (potentially order-unity dark matter fraction), sources scalar-induced GWs in two bands (peak ~10^{-8} near 3 mHz for LISA; ~10^{-11} from deci-Hz to 100 Hz for DECIGO/ET), and yields an equilateral bispectrum offset by π/2 from the power spectrum via separate-universe computation. A closed-form freeze-out transfer function is derived to cap the first two harmonics at one quarter; the high-frequency GW band is bounded by PBH overproduction, constraining friction growth. The central claim is that the shared log-period and freeze-out phase across GW bands, PBH mass, and bispectrum phase are tied to one field-localized clock and cannot be reproduced by single-scale features.

Significance. If the closed-form transfer function and phase relations hold, the work supplies a unified, analytically controlled mechanism linking potential multi-band GW signals, PBH dark matter, and non-Gaussianity through a single periodic feature. The explicit derivation of the freeze-out transfer function and harmonic bounds is a strength that enhances testability and falsifiability with LISA, DECIGO, ET, and PBH searches.

major comments (2)
  1. [model definition and thermal-channel opening] The timing and functional form of the thermal-channel opening (chosen so the friction surge affects only post-CMB scales) is load-bearing for the claim that the log-periodic structure appears exclusively at small scales while CMB scales remain untouched; the manuscript should demonstrate that the peak position, period, and phase relations persist under modest variations of this scale rather than relying on a single tuned value.
  2. [GW spectrum and PBH bound section] The statement that the high-frequency GW band is bounded by PBH overproduction (turning it into a constraint on friction growth) and that harmonics are capped at one quarter by the closed-form transfer function must be shown to be independent consequences rather than consequences of the same parameter choices that set the peak amplitude; otherwise the multi-observable correlation claim risks circularity.
minor comments (2)
  1. [Abstract] The abstract alternates between "quarter cycle" and "π/2-shifted"; adopt consistent terminology throughout for the bispectrum offset.
  2. [model section] Notation for the periodic coupling strength and thermal-channel scale should be introduced with explicit symbols in the model section to aid readability of the subsequent transfer-function derivation.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the careful reading and constructive comments on our manuscript. We address each major comment below and have revised the paper accordingly to strengthen the robustness and clarity of our claims.

read point-by-point responses

  1. Referee: [model definition and thermal-channel opening] The timing and functional form of the thermal-channel opening (chosen so the friction surge affects only post-CMB scales) is load-bearing for the claim that the log-periodic structure appears exclusively at small scales while CMB scales remain untouched; the manuscript should demonstrate that the peak position, period, and phase relations persist under modest variations of this scale rather than relying on a single tuned value.

    Authors: We agree that explicit demonstration of robustness is necessary. In the revised manuscript we have added a new subsection (with accompanying figures) that varies the thermal-channel opening scale by factors of approximately 2 around the fiducial value. The log-period, phase offset, and overall modulation structure remain stable because they are set by the periodic coupling in the friction term and the subsequent freeze-out dynamics rather than the precise onset time, provided the opening occurs after CMB scales. The peak location shifts modestly but the relations to the GW bands, PBH mass window, and bispectrum phase are preserved. revision: yes

  2. Referee: [GW spectrum and PBH bound section] The statement that the high-frequency GW band is bounded by PBH overproduction (turning it into a constraint on friction growth) and that harmonics are capped at one quarter by the closed-form transfer function must be shown to be independent consequences rather than consequences of the same parameter choices that set the peak amplitude; otherwise the multi-observable correlation claim risks circularity.

    Authors: We appreciate the referee's concern regarding potential circularity. The closed-form transfer function is obtained analytically from the curvature perturbation equation under the oscillating friction and is independent of amplitude normalization; the one-quarter harmonic cap follows directly from its functional form. The PBH overproduction bound is obtained by integrating the curvature spectrum above the collapse threshold and separately limits the allowed friction growth rate. In the revision we have added clarifying text and a short parameter scan showing that the harmonic bound holds across a range of peak amplitudes while the PBH constraint supplies an independent upper limit on growth, thereby confirming the two results are distinct consequences. revision: yes

Circularity Check

0 steps flagged

No significant circularity identified

full rationale

The paper presents a derivation of the freeze-out transfer function in closed form from the periodic coupling and thermal friction surge, then applies it to bound harmonics and constrain the high-frequency GW band via an external PBH overproduction limit. These steps are consequences of the model equations rather than inputs renamed as outputs. The central claim—that a field-localized feature produces correlated log-periodic signatures across GW bands, PBH mass, and a phase-shifted bispectrum—rests on the physical localization and timing assumptions, which are independent of the fitted parameters and do not reduce to self-definition or self-citation chains. No load-bearing prediction is shown to be equivalent to its inputs by construction, and the derivation chain remains self-contained.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

Reviewed from abstract only; explicit parameter values, full list of assumptions, and any invented entities cannot be extracted. The ledger below records the minimal elements implied by the abstract.

free parameters (2)
  • periodic coupling strength
    Amplitude of the oscillating friction term, required to produce the desired log-periodic peak height.
  • thermal-channel opening scale
    Field value at which the additional dissipation channel activates, chosen to leave CMB scales unaffected.
axioms (2)
  • domain assumption Shift-symmetric inflaton potential with periodic coupling to the thermal bath
    Invoked to allow oscillating friction without explicit breaking of shift symmetry.
  • domain assumption Standard warm-inflation background equations remain valid when the thermal channel opens
    Used as the base framework before the periodic modulation is added.

pith-pipeline@v0.9.1-grok · 5914 in / 1519 out tokens · 46209 ms · 2026-07-01T04:24:20.209338+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

103 extracted references · 71 linked inside Pith

  1. [1]

    Berera and L

    A. Berera and L. Z. Fang, Phys. Rev. Lett.74, 1912 (1995)

    1912

  2. [2]

    Berera, Phys

    A. Berera, Phys. Rev. Lett.75, 3218 (1995)

    1995

  3. [3]

    Berera, M

    A. Berera, M. Gleiser, and R. O. Ramos, Phys. Rev. D 58, 123508 (1998), arXiv:hep-ph/9803394

    Pith/arXiv arXiv 1998

  4. [4]

    Berera, I

    A. Berera, I. G. Moss, and R. O. Ramos, Rept. Prog. Phys.72, 026901 (2009), arXiv:0808.1855

    Pith/arXiv arXiv 2009

  5. [5]

    Bastero-Gil and A

    M. Bastero-Gil and A. Berera, Int. J. Mod. Phys. A24, 2207 (2009), arXiv:0902.0521

    Pith/arXiv arXiv 2009

  6. [6]

    Berera, Phys

    A. Berera, Phys. Rev. D55, 3346 (1997), arXiv:hep- ph/9612239

    arXiv 1997

  7. [7]

    Yokoyama and A

    J. Yokoyama and A. D. Linde, Phys. Rev. D60, 083509 (1999), arXiv:hep-ph/9809409

    Pith/arXiv arXiv 1999

  8. [8]

    Bastero-Gil, A

    M. Bastero-Gil, A. Berera, and R. O. Ramos, JCAP09, 033 (2011), arXiv:1008.1929

    Pith/arXiv arXiv 2011

  9. [9]

    Berera and R

    A. Berera and R. O. Ramos, Phys. Rev. D71, 023513 (2005), arXiv:hep-ph/0406339

    Pith/arXiv arXiv 2005

  10. [10]

    Berera and T

    A. Berera and T. W. Kephart, Phys. Rev. Lett.83, 1084 (1999), arXiv:hep-ph/9904410

    Pith/arXiv arXiv 1999

  11. [11]

    Laine and S

    M. Laine and S. Procacci, JCAP06, 031 (2021), arXiv:2102.09913

    arXiv 2021

  12. [12]

    Bastero-Gil, A

    M. Bastero-Gil, A. Berera, R. O. Ramos, and J. G. Rosa, Phys. Rev. Lett.117, 151301 (2016), arXiv:1604.08838

    Pith/arXiv arXiv 2016

  13. [13]

    Bastero-Gil, A

    M. Bastero-Gil, A. Berera, R. O. Ramos, and J. G. Rosa, JCAP01, 016 (2013), arXiv:1207.0445

    Pith/arXiv arXiv 2013

  14. [14]

    Bastero-Gil, A

    M. Bastero-Gil, A. Berera, R. O. Ramos, and J. G. Rosa, Phys. Lett. B813, 136055 (2021), arXiv:1907.13410

    arXiv 2021

  15. [15]

    Benetti and R

    M. Benetti and R. O. Ramos, Phys. Rev. D95, 023517 (2017), arXiv:1610.08758

    Pith/arXiv arXiv 2017

  16. [16]

    Bastero-Gil, S

    M. Bastero-Gil, S. Bhattacharya, K. Dutta, and M. R. Gangopadhyay, JCAP02, 054 (2018), arXiv:1710.10008

    Pith/arXiv arXiv 2018

  17. [17]

    Akramiet al.(Planck Collaboration), Astron

    Y. Akramiet al.(Planck Collaboration), Astron. Astro- phys.641, A10 (2020), arXiv:1807.06211

    Pith/arXiv arXiv 2020

  18. [18]

    Berera, J

    A. Berera, J. Mabillard, M. Pieroni, and R. O. Ramos, JCAP07, 021 (2018), arXiv:1803.04982

    Pith/arXiv arXiv 2018

  19. [19]

    M. R. Gangopadhyay, S. Myrzakul, M. Sami, and M. K. Sharma, Phys. Rev. D103, 043505 (2021), arXiv:2011.09155

    arXiv 2021

  20. [20]

    Basak, S

    S. Basak, S. Bhattacharya, M. R. Gangopadhyay, N. Ja- man, R. Rangarajan, and M. Sami, JCAP03, 063 (2022), arXiv:2110.00607

    arXiv 2022

  21. [21]

    Freese, J

    K. Freese, J. A. Frieman, and A. V. Olinto, Phys. Rev. Lett.65, 3233 (1990)

    1990

  22. [22]

    Silverstein and A

    E. Silverstein and A. Westphal, Phys. Rev. D78, 106003 (2008), arXiv:0803.3085

    Pith/arXiv arXiv 2008

  23. [23]

    McAllister, E

    L. McAllister, E. Silverstein, and A. Westphal, Phys. Rev. D82, 046003 (2010), arXiv:0808.0706

    Pith/arXiv arXiv 2010

  24. [24]

    Flauger, L

    R. Flauger, L. McAllister, E. Pajer, A. Westphal, and G. Xu, JCAP06, 009 (2010), arXiv:0907.2916

    Pith/arXiv arXiv 2010

  25. [25]

    Flauger and E

    R. Flauger and E. Pajer, JCAP01, 017 (2011), arXiv:1002.0833

    Pith/arXiv arXiv 2011

  26. [26]

    Hannestad, T

    S. Hannestad, T. Haugbolle, P. R. Jarnhus, and M. S. Sloth, JCAP06, 001 (2010), arXiv:0912.3527

    Pith/arXiv arXiv 2010

  27. [27]

    Flauger, L

    R. Flauger, L. McAllister, E. Silverstein, and A. West- phal, JCAP10, 055 (2017), arXiv:1412.1814

    Pith/arXiv arXiv 2017

  28. [28]

    S. R. Behbahani, A. Dymarsky, M. Mirbabayi, and L. Senatore, JCAP12, 036 (2012), arXiv:1111.3373. 15

    Pith/arXiv arXiv 2012

  29. [29]

    X. Chen, R. Easther, and E. A. Lim, JCAP04, 010 (2008), arXiv:0801.3295

    Pith/arXiv arXiv 2008

  30. [30]

    Chen, Adv

    X. Chen, Adv. Astron.2010, 638979 (2010), arXiv:1002.1416

    Pith/arXiv arXiv 2010

  31. [31]

    Kobayashi and F

    T. Kobayashi and F. Takahashi, JCAP01, 026 (2011), arXiv:1011.3988

    Pith/arXiv arXiv 2011

  32. [32]

    Ach´ ucarro, J.-O

    A. Ach´ ucarro, J.-O. Gong, S. Hardeman, G. A. Palma, and S. P. Patil, JCAP01, 030 (2011), arXiv:1010.3693

    Pith/arXiv arXiv 2011

  33. [33]

    Chen, JCAP01, 038 (2012), arXiv:1104.1323

    X. Chen, JCAP01, 038 (2012), arXiv:1104.1323

    Pith/arXiv arXiv 2012

  34. [34]

    Pajer and M

    E. Pajer and M. Peloso, Class. Quant. Grav.30, 214002 (2013), arXiv:1305.3557

    Pith/arXiv arXiv 2013

  35. [35]

    J. M. Maldacena, JHEP05, 013 (2003), arXiv:astro- ph/0210603

    arXiv 2003

  36. [36]

    Acquaviva, N

    V. Acquaviva, N. Bartolo, S. Matarrese, and A. Riotto, Nucl. Phys. B667, 119 (2003), arXiv:astro-ph/0209156

    Pith/arXiv arXiv 2003

  37. [37]

    Babich, P

    D. Babich, P. Creminelli, and M. Zaldarriaga, JCAP 08, 009 (2004), arXiv:astro-ph/0405356

    Pith/arXiv arXiv 2004

  38. [38]

    Chen, M.-x

    X. Chen, M.-x. Huang, S. Kachru, and G. Shiu, JCAP 01, 002 (2007), arXiv:hep-th/0605045

    Pith/arXiv arXiv 2007

  39. [39]

    Arya, JCAP09, 042 (2020), arXiv:1910.05238

    R. Arya, JCAP09, 042 (2020), arXiv:1910.05238

    arXiv 2020

  40. [40]

    Correa, M

    M. Correa, M. R. Gangopadhyay, N. Jaman, and G. J. Mathews, Phys. Lett. B835, 137510 (2022), arXiv:2207.10394

    arXiv 2022

  41. [41]

    Correa, M

    M. Correa, M. R. Gangopadhyay, N. Jaman, and G. J. Mathews, Phys. Rev. D109, 063539 (2024), arXiv:2306.09641

    arXiv 2024

  42. [42]

    R. Arya, R. K. Jain, and A. K. Mishra, JCAP02, 034 (2024), arXiv:2302.08940

    arXiv 2024

  43. [43]

    Ito and R

    A. Ito and R. O. Ramos, JCAP08, 076 (2025), arXiv:2504.15606

    arXiv 2025

  44. [44]

    Bastero-Gil, A

    M. Bastero-Gil, A. Berera, R. O. Ramos, and J. G. Rosa, Phys. Lett. B712, 425 (2012), arXiv:1110.3971

    Pith/arXiv arXiv 2012

  45. [45]

    J. G. Rosa and L. B. Ventura, Phys. Rev. Lett.122, 161301 (2019), arXiv:1811.05493

    Pith/arXiv arXiv 2019

  46. [46]

    K. V. Berghaus, P. W. Graham, and D. E. Kaplan, JCAP03, 034 (2020) [Erratum: JCAP10, E02 (2023)], arXiv:1910.07525

    arXiv 2020

  47. [47]

    Zell, Phys

    S. Zell, Phys. Rev. D112, L081307 (2025), arXiv:2408.07746 [hep-ph]

    arXiv 2025

  48. [48]

    Montefalcone, V

    G. Montefalcone, V. Aragam, L. Visinelli, and K. Freese, JCAP01, 032 (2024), arXiv:2306.16190

    arXiv 2024

  49. [49]

    R. O. Ramos and L. A. da Silva, JCAP03, 032 (2013), arXiv:1302.3544

    Pith/arXiv arXiv 2013

  50. [50]

    P. A. R. Adeet al.(BICEP/Keck Collaboration), Phys. Rev. Lett.127, 151301 (2021), arXiv:2110.00483

    arXiv 2021

  51. [51]

    J. E. Kim, H. P. Nilles, and M. Peloso, JCAP01, 005 (2005), arXiv:hep-ph/0409138

    Pith/arXiv arXiv 2005

  52. [52]

    Graham and I

    C. Graham and I. G. Moss, JCAP07, 013 (2009), arXiv:0905.3500

    Pith/arXiv arXiv 2009

  53. [53]

    Bastero-Gil, A

    M. Bastero-Gil, A. Berera, I. G. Moss, and R. O. Ramos, JCAP05, 004 (2014), arXiv:1401.1149

    Pith/arXiv arXiv 2014

  54. [54]

    Visinelli, JCAP01, 005 (2015), arXiv:1410.1187

    L. Visinelli, JCAP01, 005 (2015), arXiv:1410.1187

    Pith/arXiv arXiv 2015

  55. [55]

    Bastero-Gil, A

    M. Bastero-Gil, A. Berera, and R. O. Ramos, JCAP07, 030 (2011), arXiv:1106.0701

    Pith/arXiv arXiv 2011

  56. [56]

    Bastero-Gil, A

    M. Bastero-Gil, A. Berera, R. Brandenberger, I. G. Moss, R. O. Ramos, and J. G. Rosa, JCAP 01, 002 (2018), arXiv:1612.04726

    Pith/arXiv arXiv 2018

  57. [57]

    M. R. Gangopadhyay, J. C. Jain, D. Sharma, and Yo- gesh, Eur. Phys. J. C82, 849 (2022), arXiv:2108.13839

    arXiv 2022

  58. [58]

    Choudhury, M

    S. Choudhury, M. R. Gangopadhyay, and M. Sami, Eur. Phys. J. C84, 884 (2024), arXiv:2301.10000

    arXiv 2024

  59. [59]

    M. R. Gangopadhyay and N. Kumar, Phys. Dark Univ. 52(2026), arXiv:2603.11629

    Pith/arXiv arXiv 2026

  60. [60]

    W. H. Press and P. Schechter, Astrophys. J.187, 425 (1974)

    1974

  61. [61]

    B. J. Carr and S. W. Hawking, Mon. Not. R. Astron. Soc.168, 399 (1974)

    1974

  62. [62]

    B. J. Carr, Astrophys. J.201, 1 (1975)

    1975

  63. [63]

    A. M. Green and B. J. Kavanagh, J. Phys. G48, 043001 (2021), arXiv:2007.10722

    Pith/arXiv arXiv 2021

  64. [64]

    Musco, Phys

    I. Musco, Phys. Rev. D100, 123524 (2019), arXiv:1809.02127

    arXiv 2019

  65. [65]

    Harada, C.-M

    T. Harada, C.-M. Yoo, and K. Kohri, Phys. Rev. D 88, 084051 (2013) [Erratum: Phys. Rev. D89, 029903 (2014)], arXiv:1309.4201

    Pith/arXiv arXiv 2013

  66. [66]

    J. C. Niemeyer and K. Jedamzik, Phys. Rev. D59, 124013 (1999), arXiv:astro-ph/9901292

    Pith/arXiv arXiv 1999

  67. [67]

    Shibata and M

    M. Shibata and M. Sasaki, Phys. Rev. D60, 084002 (1999), arXiv:gr-qc/9905064

    Pith/arXiv arXiv 1999

  68. [68]

    Young, C

    S. Young, C. T. Byrnes, and M. Sasaki, JCAP07, 045 (2014), arXiv:1405.7023

    Pith/arXiv arXiv 2014

  69. [69]

    B. Carr, K. Kohri, Y. Sendouda, and J. Yokoyama, Rept. Prog. Phys.84, 116902 (2021), arXiv:2002.12778

    Pith/arXiv arXiv 2021

  70. [70]

    Niikuraet al., Nat

    H. Niikuraet al., Nat. Astron.3, 524 (2019), arXiv:1701.02151

    Pith/arXiv arXiv 2019

  71. [71]

    Niikura, M

    H. Niikura, M. Takada, S. Yokoyama, T. Sumi, and S. Masaki, Phys. Rev. D99, 083503 (2019), arXiv:1901.07120

    Pith/arXiv arXiv 2019

  72. [72]

    Carr and F

    B. Carr and F. K¨ uhnel, Ann. Rev. Nucl. Part. Sci.70, 355 (2020), arXiv:2006.02838

    Pith/arXiv arXiv 2020

  73. [73]

    Sasaki, T

    M. Sasaki, T. Suyama, T. Tanaka, and S. Yokoyama, Class. Quant. Grav.35, 063001 (2018), arXiv:1801.05235

    Pith/arXiv arXiv 2018

  74. [74]

    B. Carr, F. K¨ uhnel, and M. Sandstad, Phys. Rev. D94, 083504 (2016), arXiv:1607.06077

    Pith/arXiv arXiv 2016

  75. [75]

    B. Carr, F. K¨ uhnel, and L. Visinelli, Mon. Not. R. As- tron. Soc.501, 2029 (2021), arXiv:2008.08077

    arXiv 2029

  76. [76]

    M. W. Choptuik, Phys. Rev. Lett.70, 9 (1993)

    1993

  77. [77]

    C.-M. Yoo, T. Harada, J. Garriga, and K. Kohri, PTEP 2018, 123E01 (2018), arXiv:1805.03946

    arXiv 2018

  78. [78]

    Atal and C

    V. Atal and C. Germani, Phys. Dark Univ.24, 100275 (2019), arXiv:1811.07857

    Pith/arXiv arXiv 2019

  79. [79]

    K. N. Ananda, C. Clarkson, and D. Wands, Phys. Rev. D75, 123518 (2007), arXiv:gr-qc/0612013

    Pith/arXiv arXiv 2007

  80. [80]

    Baumann, P

    D. Baumann, P. J. Steinhardt, K. Takahashi, and K. Ichiki, Phys. Rev. D76, 084019 (2007), arXiv:hep- th/0703290

    arXiv 2007

Showing first 80 references.