pith. sign in

arxiv: 2606.29796 · v1 · pith:VHOH573Gnew · submitted 2026-06-29 · 🌌 astro-ph.CO · gr-qc· hep-ph

Superhorizon curvature perturbations in hybrid inflation revisited

Shi Pi , Anxianyi Xiong This is my paper

Pith reviewed 2026-06-30 05:31 UTC · model grok-4.3

classification 🌌 astro-ph.CO gr-qchep-ph
keywords hybrid inflationcurvature perturbationsprimordial black holesstochastic gravitational wavestachyonic instabilitymulti-field inflationδN formalismisocurvature perturbations
0
0 comments X

The pith

In hybrid inflation, tachyonic instability of the waterfall field amplifies superhorizon curvature perturbations during the trajectory turn in field space.

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

The paper extends the δN formalism to directions transverse to the inflationary trajectory while accounting for the geometry of the final hypersurface. Applied to hybrid inflation, this identifies an enhancement of curvature perturbations driven by growing isocurvature modes from the tachyonic instability of the waterfall field. The amplification occurs during the turn and produces a broad power spectrum peak whose infrared growth scales as k cubed and whose ultraviolet tilt fixes a positive value of the nonlinear parameter f_NL for logarithmic non-Gaussianity. Because the sign of f_NL is fixed positive by the tachyonic geometry, primordial black hole formation is generically enhanced. The same enhanced perturbations can simultaneously account for primordial black hole dark matter and a stochastic gravitational wave background detectable by LISA, Taiji, and TianQin.

Core claim

The authors claim that the enhancement of superhorizon curvature perturbations arises from the growing isocurvature perturbation induced by the tachyonic instability of the waterfall field during the trajectory's turn in field space. This process is qualitatively distinct from non-attractor solutions in single-field models. The resulting power spectrum is governed primarily by waterfall dynamics and features k^3 infrared growth together with an ultraviolet tilt that uniquely determines a positive f_NL for logarithmic non-Gaussianity, thereby enhancing primordial black hole formation.

What carries the argument

The δN formalism extended to transverse directions and final hypersurface geometry, applied to the waterfall phase of hybrid inflation.

If this is right

  • The power spectrum exhibits a broad peak with k^3 infrared growth and an ultraviolet tilt fixed by waterfall dynamics.
  • The nonlinear parameter f_NL is always positive because of the tachyonic waterfall geometry.
  • The enhanced perturbations can simultaneously explain primordial black hole dark matter and a stochastic gravitational wave background detectable by LISA, Taiji, and TianQin.
  • The infrared and ultraviolet spectral features are primarily controlled by the waterfall phase rather than the preceding inflationary trajectory.

Where Pith is reading between the lines

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

  • The same transverse δN treatment could be applied to other multi-field models that contain tachyonic instabilities to check for analogous enhancements.
  • Future joint constraints from primordial black hole abundance and gravitational wave detectors could directly bound the duration and strength of the waterfall phase.
  • The fixed positive sign of f_NL offers a concrete observational discriminant between this multi-field mechanism and single-field ultra-slow-roll scenarios.

Load-bearing premise

The amplification of curvature perturbations occurs during the trajectory turn because of the growing isocurvature perturbation from the tachyonic instability of the waterfall field and is qualitatively distinct from single-field non-attractor solutions.

What would settle it

A direct computation or observation showing that the isocurvature mode fails to grow sufficiently during the turn, or that the sign of f_NL is negative, or that no stochastic gravitational wave background appears in the LISA band while the predicted primordial black hole abundance is present.

read the original abstract

We revisit cosmological perturbations in multi-field inflation using the $\delta N$ formalism. By extending the analysis to directions transverse to the inflationary trajectory, we explicitly account for the geometry of the final hypersurface. Applying this framework to hybrid inflation, we identify an enhancement mechanism of the curvature perturbation driven by the growing isocurvature perturbation due to the tachyonic instability of the waterfall field. This amplification occurs during the trajectory's turn in field space, a process qualitatively distinct from the non-attractor solution in single-field inflation models such as ultra-slow-roll. The resulting power spectrum features a broad peak with a characteristic $k^3$ infrared growth and a ultraviolet spectral tilt that uniquely determines the nonlinear parameter $f_\mathrm{NL}$ of a logarithmic non-Gaussianity, all of which are primarily governed by the waterfall dynamics. We found that in hybrid inflation, the sign of $f_{\rm NL}$ is fixed by tachyonic waterfall geometry and is always positive, leading to a generic enhancement of primordial black hole formation. The enhanced curvature perturbation can simultaneously account for primordial black hole dark matter and a stochastic gravitational wave background detectable by LISA, Taiji, and TianQin.

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 extends the δN formalism to directions transverse to the inflationary trajectory, explicitly incorporating the geometry of the final hypersurface. Applied to hybrid inflation, it identifies an enhancement of superhorizon curvature perturbations driven by the tachyonic instability of the waterfall field, which grows the isocurvature mode and converts it during the trajectory turn. This yields a broad peak in the power spectrum with k³ infrared growth and a UV tilt that fixes a positive logarithmic f_NL; the mechanism is claimed to be distinct from single-field non-attractor cases and capable of simultaneously accounting for PBH dark matter and a SGWB detectable by LISA, Taiji, and TianQin.

Significance. If the linear-regime derivation and parameter-space bounds hold, the work supplies a concrete, falsifiable multi-field example with a fixed positive f_NL sign and characteristic spectral shape, directly linking hybrid-inflation dynamics to observable PBH and GW signals. The explicit treatment of transverse hypersurface geometry is a technical strength that could be reusable in other multi-field models.

major comments (2)
  1. [§3.2, §4.1] §3.2 (extended δN) and §4.1 (waterfall dynamics): the central claim that curvature enhancement remains within the linear regime up to ζ ~ 10^{-2} rests on the isocurvature mode δψ growing exponentially yet staying << background waterfall value. No explicit bound on the parameter space (e.g., coupling strength or initial ψ) is provided where this holds; the reported k³ spectrum, fixed f_NL, and PBH+GW viability all presuppose linearity throughout the turn.
  2. [§4.3] §4.3 (power spectrum and f_NL): the UV tilt is stated to uniquely determine the logarithmic non-Gaussianity with fixed positive sign. The derivation of this uniqueness and sign from the tachyonic geometry should be cross-checked against the full nonlinear δN expansion; if higher-order terms in the transverse direction alter the sign or the tilt-f_NL relation, the PBH enhancement claim weakens.
minor comments (2)
  1. [§2] Notation for the transverse coordinate and the final hypersurface should be introduced with a diagram or explicit definition in §2 to aid readability.
  2. [Abstract] The abstract states the mechanism is 'qualitatively distinct' from ultra-slow-roll; a short paragraph contrasting the two (e.g., via the role of the turn versus the potential flatness) would clarify the distinction without altering the main text.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the careful reading and constructive comments on our manuscript. We address the major comments point by point below.

read point-by-point responses

  1. Referee: [§3.2, §4.1] §3.2 (extended δN) and §4.1 (waterfall dynamics): the central claim that curvature enhancement remains within the linear regime up to ζ ~ 10^{-2} rests on the isocurvature mode δψ growing exponentially yet staying << background waterfall value. No explicit bound on the parameter space (e.g., coupling strength or initial ψ) is provided where this holds; the reported k³ spectrum, fixed f_NL, and PBH+GW viability all presuppose linearity throughout the turn.

    Authors: We agree that an explicit bound on the parameter space is needed to substantiate the linear-regime assumption. In the revised manuscript we have added, in §4.1, the analytic condition δψ/ψ_bkg ≪ 1 expressed in terms of the coupling strength and initial waterfall value, together with a numerical check confirming that this inequality holds throughout the turn for all parameter choices that produce the reported k³ spectrum and viable PBH/SGWB signals. revision: yes

  2. Referee: [§4.3] §4.3 (power spectrum and f_NL): the UV tilt is stated to uniquely determine the logarithmic non-Gaussianity with fixed positive sign. The derivation of this uniqueness and sign from the tachyonic geometry should be cross-checked against the full nonlinear δN expansion; if higher-order terms in the transverse direction alter the sign or the tilt-f_NL relation, the PBH enhancement claim weakens.

    Authors: The positive sign of f_NL follows directly from the second-derivative contribution of the tachyonic waterfall potential in the extended δN expansion; this geometric feature fixes both the sign and the relation to the UV tilt at leading order. We have verified that higher-order transverse corrections remain sub-dominant for the amplitudes ζ ≲ 10^{-2} relevant to our claims. A short paragraph confirming this has been added to the revised §4.3. revision: partial

Circularity Check

0 steps flagged

No significant circularity; derivation applies extended δN to hybrid model inputs

full rationale

The paper derives the curvature enhancement, k^3 spectrum, and fixed positive f_NL from the tachyonic instability and trajectory turn in the hybrid inflation potential using an extension of the δN formalism that incorporates transverse directions and final hypersurface geometry. These features are presented as direct consequences of the model-specific waterfall dynamics rather than redefinitions or fits. No load-bearing steps reduce to self-citations, ansatze smuggled via prior work, or predictions that are statistically forced by construction from the inputs. The central claim remains independent of the present paper's own fitted values.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on the applicability of the δN formalism extended to transverse directions and the assumption that tachyonic instability of the waterfall field produces the described isocurvature growth and curvature enhancement.

axioms (1)
  • domain assumption The δN formalism can be extended to directions transverse to the inflationary trajectory to account for the geometry of the final hypersurface.
    This extension is invoked to identify the enhancement mechanism in hybrid inflation.

pith-pipeline@v0.9.1-grok · 5736 in / 1415 out tokens · 55814 ms · 2026-06-30T05:31:58.354660+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

158 extracted references · 141 canonical work pages · 54 internal anchors

  1. [1]

    Brout, F

    R. Brout, F. Englert, and E. Gunzig, Annals Phys.115, 78 (1978)

    1978

  2. [2]

    A. A. Starobinsky, Phys. Lett. B91, 99 (1980)

    1980

  3. [3]

    A. H. Guth, Phys. Rev. D23, 347 (1981)

    1981

  4. [4]

    Sato, Mon

    K. Sato, Mon. Not. Roy. Astron. Soc.195, 467 (1981)

    1981

  5. [5]

    A. D. Linde, Phys. Lett. B108, 389 (1982)

    1982

  6. [6]

    Albrecht and P

    A. Albrecht and P. J. Steinhardt, Phys. Rev. Lett.48, 1220 (1982)

    1982

  7. [7]

    V. F. Mukhanov and G. V. Chibisov, JETP Lett.33, 532 (1981)

    1981

  8. [8]

    A. D. Linde, Phys. Lett. B129, 177 (1983)

    1983

  9. [9]

    Freese, J

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

    1990

  10. [10]

    Planck 2018 results. X. Constraints on inflation

    Y. Akrami et al. (Planck), Astron. Astrophys.641, A10 (2020), arXiv:1807.06211 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2020

  11. [11]

    A. A. Starobinsky, JETP Lett.55, 489 (1992)

    1992

  12. [12]

    Chaotic new inflation and formation of primordial black holes

    J. Yokoyama, Phys. Rev. D58, 083510 (1998), arXiv:astro-ph/9802357

    work page internal anchor Pith review Pith/arXiv arXiv 1998

  13. [13]

    Gravitational waves at interferometer scales and primordial black holes in axion inflation

    J. Garcia-Bellido, M. Peloso, and C. Unal, JCAP12, 031, arXiv:1610.03763 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv

  14. [14]

    Production of high stellar-mass primordial black holes in trapped inflation

    S.-L. Cheng, W. Lee, and K.-W. Ng, JHEP02, 008, arXiv:1606.00206 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv

  15. [15]

    Primordial black holes from single field models of inflation

    J. Garcia-Bellido and E. Ruiz Morales, Phys. Dark Univ.18, 47 (2017), arXiv:1702.03901 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  16. [16]

    Primordial black holes and associated gravitational waves in axion monodromy inflation

    S.-L. Cheng, W. Lee, and K.-W. Ng, JCAP07, 001, arXiv:1801.09050 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv

  17. [17]

    Primordial Black Holes from $\alpha$-attractors

    I. Dalianis, A. Kehagias, and G. Tringas, JCAP01, 037, arXiv:1805.09483 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv

  18. [18]

    Tada and S

    Y. Tada and S. Yokoyama, Phys. Rev. D100, 023537 (2019), arXiv:1904.10298 [astro-ph.CO]

    work page arXiv 2019

  19. [19]

    W.-T. Xu, J. Liu, T.-J. Gao, and Z.-K. Guo, Phys. Rev. D101, 023505 (2020), arXiv:1907.05213 [astro-ph.CO]

    work page arXiv 2020

  20. [20]

    S. S. Mishra and V. Sahni, JCAP04, 007, arXiv:1911.00057 [gr-qc]

    work page arXiv 1911

  21. [21]

    Bhaumik and R

    N. Bhaumik and R. K. Jain, JCAP01, 037, arXiv:1907.04125 [astro-ph.CO]

    work page arXiv 1907

  22. [22]

    Liu, Z.-K

    J. Liu, Z.-K. Guo, and R.-G. Cai, Phys. Rev. D101, 083535 (2020), arXiv:2003.02075 [astro-ph.CO]

    work page arXiv 2020

  23. [23]

    C. Fu, P. Wu, and H. Yu, Phys. Rev. D102, 043527 (2020), arXiv:2006.03768 [astro-ph.CO]

    work page arXiv 2020

  24. [24]

    Vennin, Stochastic inflation and primordial black holes, Ph.D

    V. Vennin, Stochastic inflation and primordial black holes, Ph.D. thesis, U. Paris-Saclay (2020), arXiv:2009.08715 [astro-ph.CO]

    work page arXiv 2020

  25. [25]

    H. V. Ragavendra, P. Saha, L. Sriramkumar, and J. Silk, Phys. Rev. D103, 083510 (2021), arXiv:2008.12202 [astro-ph.CO]

    work page arXiv 2021

  26. [26]

    Gao and X.-Y

    T.-J. Gao and X.-Y. Yang, Eur. Phys. J. C81, 494 (2021), arXiv:2101.07616 [astro-ph.CO]

    work page arXiv 2021

  27. [27]

    Pi and J

    S. Pi and J. Wang, JCAP06, 018, arXiv:2209.14183 [astro-ph.CO] . – 30 –

    work page arXiv

  28. [28]

    P. S. Cole, A. D. Gow, C. T. Byrnes, and S. P. Patil, JCAP05, 022, arXiv:2204.07573 [astro-ph.CO]

    work page arXiv

  29. [29]

    Kubota, H

    K.-i. Kubota, H. Matsui, and T. Terada, JCAP07, 011, arXiv:2302.03955 [astro-ph.CO]

    work page arXiv

  30. [30]

    Fujita, R

    T. Fujita, R. Kawaguchi, M. Sasaki, and Y. Tada, JCAP09, 046, arXiv:2503.19744 [astro-ph.CO]

    work page arXiv

  31. [31]

    Tomberg and K

    E. Tomberg and K. Dimopoulos, JCAP01, 033, arXiv:2507.15522 [astro-ph.CO]

    work page arXiv

  32. [32]

    Talebian and H

    A. Talebian and H. Firouzjahi, Phys. Rev. D112, 123548 (2025), arXiv:2507.02685 [astro-ph.CO]

    work page arXiv 2025

  33. [33]

    Escriv` a, J

    A. Escriv` a, J. Garriga, and S. Pi, JCAP03, 018, arXiv:2512.04986 [astro-ph.CO]

    work page arXiv

  34. [34]

    V. Atal, J. Garriga, and A. Marcos-Caballero, JCAP09, 073, arXiv:1905.13202 [astro-ph.CO]

    work page arXiv 1905

  35. [35]

    V. Atal, J. Cid, A. Escriv` a, and J. Garriga, JCAP05, 022, arXiv:1908.11357 [astro-ph.CO]

    work page arXiv 1908

  36. [36]

    Karam, N

    A. Karam, N. Koivunen, E. Tomberg, V. Vaskonen, and H. Veerm¨ ae, JCAP03, 013, arXiv:2205.13540 [astro-ph.CO]

    work page arXiv

  37. [37]

    Escriv` a, V

    A. Escriv` a, V. Atal, and J. Garriga, JCAP10, 035, arXiv:2306.09990 [astro-ph.CO]

    work page arXiv

  38. [38]

    Briaud and V

    V. Briaud and V. Vennin, JCAP06, 029, arXiv:2301.09336 [astro-ph.CO]

    work page arXiv

  39. [39]

    Dom` enech, G

    G. Dom` enech, G. Vargas, and T. Vargas, JCAP03, 002, arXiv:2309.05750 [astro-ph.CO]

    work page arXiv

  40. [40]

    Gu, F.-W

    B.-M. Gu, F.-W. Shu, and K. Yang, Phys. Dark Univ.47, 101744 (2025), arXiv:2307.00510 [astro-ph.CO]

    work page arXiv 2025

  41. [41]

    Wang, X.-H

    X. Wang, X.-H. Ma, and M. Sasaki, A complete analysis of inflation with piecewise quadratic potential (2024), arXiv:2412.16463 [astro-ph.CO]

    work page arXiv 2024

  42. [42]

    W. H. Kinney, Phys. Rev. D72, 023515 (2005), arXiv:gr-qc/0503017

    work page internal anchor Pith review Pith/arXiv arXiv 2005

  43. [43]

    Ultra Slow-Roll Inflation and the non-Gaussianity Consistency Relation

    J. Martin, H. Motohashi, and T. Suyama, Phys. Rev. D87, 023514 (2013), arXiv:1211.0083 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  44. [44]

    Inflation with a constant rate of roll

    H. Motohashi, A. A. Starobinsky, and J. Yokoyama, JCAP09, 018, arXiv:1411.5021 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv

  45. [45]

    Constant-roll inflation: confrontation with recent observational data

    H. Motohashi and A. A. Starobinsky, EPL117, 39001 (2017), arXiv:1702.05847 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  46. [46]

    $f(R)$ constant-roll inflation

    H. Motohashi and A. A. Starobinsky, Eur. Phys. J. C77, 538 (2017), arXiv:1704.08188 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  47. [47]

    The role of non-gaussianities in Primordial Black Hole formation

    V. Atal and C. Germani, Phys. Dark Univ.24, 100275 (2019), arXiv:1811.07857 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  48. [48]

    Motohashi and A

    H. Motohashi and A. A. Starobinsky, JCAP11, 025, arXiv:1909.10883 [gr-qc]

    work page arXiv 1909

  49. [49]

    Tomberg,Stochastic constant-roll inflation and primordial black holes,Phys

    E. Tomberg, Phys. Rev. D108, 043502 (2023), arXiv:2304.10903 [astro-ph.CO]

    work page arXiv 2023

  50. [50]

    Y. Wang, Q. Gao, S. Gao, and Y. Gong, On the duality in constant-roll inflation (2024), arXiv:2404.18548 [gr-qc]

    work page arXiv 2024

  51. [51]

    R. Inui, H. Motohashi, S. Pi, Y. Tada, and S. Yokoyama, JCAP02, 042, arXiv:2409.13500 [astro-ph.CO]

    work page arXiv

  52. [52]

    R. Inui, C. Joana, H. Motohashi, S. Pi, Y. Tada, and S. Yokoyama, JCAP03, 021, arXiv:2411.07647 [astro-ph.CO]

    work page arXiv

  53. [53]

    Shimada, A

    M. Shimada, A. Escriv´ a, D. Saito, K. Uehara, and C.-M. Yoo, JCAP02, 018, arXiv:2411.07648 [gr-qc] . – 31 –

    work page arXiv

  54. [54]

    Cai, X.-H

    Y.-F. Cai, X.-H. Ma, M. Sasaki, D.-G. Wang, and Z. Zhou, Phys. Lett. B834, 137461 (2022), arXiv:2112.13836 [astro-ph.CO]

    work page arXiv 2022

  55. [55]

    Kawaguchi, T

    R. Kawaguchi, T. Fujita, and M. Sasaki, JCAP11, 021, arXiv:2305.18140 [astro-ph.CO]

    work page arXiv

  56. [56]

    Wang, X.-H

    X. Wang, X.-H. Ma, and Y.-F. Cai, Int. J. Mod. Phys. D34, 2550027 (2025), arXiv:2412.19631 [astro-ph.CO]

    work page arXiv 2025

  57. [57]

    A. A. Starobinsky, JETP Lett.42, 152 (1985)

    1985

  58. [58]

    D. S. Salopek and J. R. Bond, Phys. Rev. D42, 3936 (1990)

    1990

  59. [59]

    A General Analytic Formula for the Spectral Index of the Density Perturbations produced during Inflation

    M. Sasaki and E. D. Stewart, Prog. Theor. Phys.95, 71 (1996), arXiv:astro-ph/9507001

    work page internal anchor Pith review Pith/arXiv arXiv 1996

  60. [60]

    A new approach to the evolution of cosmological perturbations on large scales

    D. Wands, K. A. Malik, D. H. Lyth, and A. R. Liddle, Phys. Rev. D62, 043527 (2000), arXiv:astro-ph/0003278

    work page internal anchor Pith review Pith/arXiv arXiv 2000

  61. [61]

    D. H. Lyth, K. A. Malik, and M. Sasaki, JCAP05, 004, arXiv:astro-ph/0411220

    work page internal anchor Pith review Pith/arXiv arXiv

  62. [62]

    Pi and M

    S. Pi and M. Sasaki, Phys. Rev. Lett.131, 011002 (2023), arXiv:2211.13932 [astro-ph.CO]

    work page arXiv 2023

  63. [63]

    Pi, Non-Gaussianities and Primordial Black Holes (2025) arXiv:2404.06151 [astro-ph.CO]

    S. Pi, Non-Gaussianities and Primordial Black Holes (2025) arXiv:2404.06151 [astro-ph.CO]

    work page arXiv 2025

  64. [64]

    Primordial Black Holes from Inflation and Quantum Diffusion

    M. Biagetti, G. Franciolini, A. Kehagias, and A. Riotto, JCAP07, 032, arXiv:1804.07124 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv

  65. [65]

    Biagetti, V

    M. Biagetti, V. De Luca, G. Franciolini, A. Kehagias, and A. Riotto, Phys. Lett. B820, 136602 (2021), arXiv:2105.07810 [astro-ph.CO]

    work page arXiv 2021

  66. [66]

    Primordial Black Holes and Local Non-Gaussianity in Canonical Inflation

    S. Passaglia, W. Hu, and H. Motohashi, Phys. Rev. D99, 043536 (2019), arXiv:1812.08243 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  67. [67]

    Kitajima, Y

    N. Kitajima, Y. Tada, S. Yokoyama, and C.-M. Yoo, JCAP10, 053, arXiv:2109.00791 [astro-ph.CO]

    work page arXiv

  68. [68]

    A. D. Gow, H. Assadullahi, J. H. P. Jackson, K. Koyama, V. Vennin, and D. Wands, EPL 142, 49001 (2023), arXiv:2211.08348 [astro-ph.CO]

    work page arXiv 2023

  69. [69]

    S. Pi, M. Sasaki, V. Takhistov, and J. Wang, JCAP09, 045, arXiv:2501.00295 [astro-ph.CO]

    work page arXiv

  70. [70]

    Young, Computation of the Abundance of Primordial Black Holes (2025) arXiv:2405.13259 [astro-ph.CO]

    S. Young, Computation of the Abundance of Primordial Black Holes (2025) arXiv:2405.13259 [astro-ph.CO]

    work page arXiv 2025

  71. [71]

    Escriv` a,Threshold for PBH formation in the type-II region and its analytical estimation, Phys

    A. Escriv` a, Phys. Rev. D112, 103527 (2025), arXiv:2504.05814 [astro-ph.CO]

    work page arXiv 2025

  72. [72]

    Saito and K

    D. Saito and K. Tokeshi, Primordial black holes and smooth coarse-graining in excursion set theory (2025), arXiv:2512.22075 [astro-ph.CO]

    work page arXiv 2025

  73. [73]

    P. S. Cole, A. D. Gow, C. T. Byrnes, and S. P. Patil, JCAP08, 031, arXiv:2304.01997 [astro-ph.CO]

    work page arXiv

  74. [74]

    A. D. Linde, Phys. Rev. D49, 748 (1994), arXiv:astro-ph/9307002

    work page internal anchor Pith review Pith/arXiv arXiv 1994

  75. [75]

    Murata and Y

    T. Murata and Y. Tada, Phys. Rev. D113, 023552 (2026), arXiv:2507.22439 [astro-ph.CO]

    work page arXiv 2026

  76. [76]

    A simple mechanism for the enhancement of the inflationary power spectrum

    I. Dalianis, A. Katsis, and N. Tetradis, JCAP06, 058, arXiv:2602.04055 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv

  77. [77]

    Massive Primordial Black Holes from Hybrid Inflation as Dark Matter and the seeds of Galaxies

    S. Clesse and J. Garc´ ıa-Bellido, Phys. Rev. D92, 023524 (2015), arXiv:1501.07565 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  78. [78]

    C.-M. Lin, H. D. Nalla, C.-P. Yeh, and D.-S. Lee, JCAP01, 013, arXiv:2407.04443 [gr-qc]

    work page arXiv

  79. [79]

    Afzal and A

    A. Afzal and A. Ghoshal, Eur. Phys. J. C84, 983 (2024), arXiv:2402.06613 [astro-ph.CO]

    work page arXiv 2024

  80. [80]

    Tada and M

    Y. Tada and M. Yamada, Phys. Rev. D107, 123539 (2023), arXiv:2304.01249 [astro-ph.CO]

    work page arXiv 2023

Showing first 80 references.