pith. sign in

arxiv: 2510.09395 · v3 · pith:XJI7HW2Jnew · submitted 2025-10-10 · ✦ hep-ph · gr-qc· hep-th

Dark matter production from evaporation of regular primordial black holes

Ngo Phuc Duc Loc This is my paper

Pith reviewed 2026-05-22 12:37 UTC · model grok-4.3

classification ✦ hep-ph gr-qchep-th
keywords regular black holesprimordial black holesdark matter productionevaporationHawking radiationself-similarityHayward metricSimpson-Visser metric
0
0 comments X

The pith

Redefining the regularization parameter lets regular black holes evaporate completely like singular ones.

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

The paper shows that a straightforward redefinition of the regularizing parameter in regular black hole metrics keeps the evaporation process self-similar. This means regular black holes can disappear entirely through Hawking radiation, just as singular black holes do, avoiding the need for exotic remnants. Building on this, the authors outline a framework for how the evaporation of regular primordial black holes could generate dark matter, with examples using the Hayward and Simpson-Visser metrics yielding different temperatures, sizes, and lifetimes that adjust the constraints for matching the observed dark matter density.

Core claim

By redefining the regularizing parameter, regular black hole metrics maintain self-similarity during evaporation, allowing complete evaporation and the production of dark matter from regular primordial black holes. For the Hayward and Simpson-Visser cases, the distinct Hawking temperatures and horizon sizes lead to altered mass evolution and lifetime, resulting in modified cosmological constraints on the parameter space that can reproduce the correct dark matter abundance.

What carries the argument

Redefinition of the regularizing parameter in regular black hole metrics to preserve evaporation self-similarity

If this is right

  • Regular primordial black holes evaporate completely without leaving remnants such as horizonless objects or wormholes.
  • The lifetime and mass evolution of regular primordial black holes differ from singular ones due to modified temperature and horizon size.
  • Cosmological constraints on dark matter production from black hole evaporation are adjusted for each regular metric.
  • The general framework applies to other regular black hole metrics beyond the illustrative examples.

Where Pith is reading between the lines

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

  • This approach could link the resolution of black hole singularities directly to the source of dark matter in a single mechanism.
  • Observations of early-universe relics or gamma-ray backgrounds could test the modified mass ranges for dark matter production.

Load-bearing premise

The redefinition of the regularization parameter keeps the spacetime metric consistent and allows the standard Hawking radiation formula to apply without introducing instabilities or violating energy conditions during the full evaporation process.

What would settle it

A calculation demonstrating that the redefined parameter causes metric inconsistencies or energy condition violations at some evaporation stage would falsify the complete-evaporation claim.

Figures

Figures reproduced from arXiv: 2510.09395 by Ngo Phuc Duc Loc.

Figure 1
Figure 1. Figure 1: FIG. 1: Schematic sketch comparing Hawking temperature of s [PITH_FULL_IMAGE:figures/full_fig_p006_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2 [PITH_FULL_IMAGE:figures/full_fig_p009_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3: BBN constraint on RPBH mass as a function of [PITH_FULL_IMAGE:figures/full_fig_p015_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4: Warm DM constraint on RPBH mass as a function of DM mass [PITH_FULL_IMAGE:figures/full_fig_p016_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5 [PITH_FULL_IMAGE:figures/full_fig_p018_5.png] view at source ↗
read the original abstract

We point out that a simple redefinition of the regularizing parameter in regular black hole (RBH) metrics can preserve the self-similarity of the evaporation process. This implies that a RBH can evaporate completely, mirroring the behavior of its singular counterpart. Consequently, RBHs need not evolve into exotic, unverified remnant states such as horizonless compact objects or wormholes. We then provide a general framework to study dark matter (DM) production from evaporation of regular primordial black holes (RPBHs). As illustrative examples, we explicitly work out the cases of the Hayward metric and the Simpson-Visser metric. The formalism can be readily applied to other metrics. RPBH generally exhibits different Hawking temperature and horizon size compared to their singular counterpart, leading to distinct lifetime and mass evolution. We calculate the resulting modified cosmological constraints and the allowed parameter space to obtain the correct DM abundance. This intriguing scenario provides a unified resolution to both the DM problem and the black hole singularity problem, while preserving the standard self-similar evaporation process.

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 claims that redefining the regularization parameter (e.g., making it scale with instantaneous mass M) in regular black hole metrics such as Hayward and Simpson-Visser preserves the self-similarity of the evaporation process. This allows regular primordial black holes to evaporate completely, like singular ones, without forming remnants. The authors then develop a general framework for dark matter production via Hawking radiation from these evaporating RPBHs, compute modified lifetimes and mass evolution, and derive cosmological constraints on the parameter space (initial mass and regularization scale) that yield the observed DM abundance.

Significance. If the central redefinition is shown to be consistent, the work would provide a unified resolution to the black hole singularity problem and the dark matter problem by permitting complete evaporation of regular PBHs while generating distinct Hawking temperatures and horizon radii that alter DM yield and cosmological bounds. The explicit treatment of Hayward and Simpson-Visser cases, plus the general framework applicable to other metrics, adds concrete value.

major comments (2)
  1. [Sections on metric redefinition and evaporation (Hayward and Simpson-Visser cases)] The redefinition of the regularization parameter l to scale with instantaneous M (discussed for Hayward and Simpson-Visser metrics) is asserted to preserve the exact static metric form and the standard Hawking temperature T = (1/4π) f'(r_h) throughout evaporation. However, no derivation is provided showing that the resulting time-dependent metric satisfies the Einstein equations with a physically reasonable, time-dependent stress-energy tensor that continues to obey the null energy condition near the would-be singularity as M decreases. This is load-bearing for the self-similarity claim and the applicability of the semiclassical radiation formula used in the DM yield calculation.
  2. [DM production and cosmological constraints section] The allowed parameter space for M_i and l is obtained by requiring the integrated DM yield to equal the observed abundance. This defines the viable region by fitting to the target result rather than producing an independent, falsifiable prediction from the modified temperature and horizon size; the resulting cosmological constraints are therefore weaker than presented.
minor comments (2)
  1. [Abstract] The abstract states that RPBHs exhibit 'different Hawking temperature and horizon size' but does not quantify the leading-order differences relative to Schwarzschild; adding a brief explicit comparison would improve readability.
  2. [General] Notation for the time-dependent regularization parameter (l(M)) should be introduced with a clear equation when first used, to avoid ambiguity in later mass-evolution formulas.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the careful reading of our manuscript and the constructive comments. We address each of the major comments below.

read point-by-point responses

  1. Referee: The redefinition of the regularization parameter l to scale with instantaneous M (discussed for Hayward and Simpson-Visser metrics) is asserted to preserve the exact static metric form and the standard Hawking temperature T = (1/4π) f'(r_h) throughout evaporation. However, no derivation is provided showing that the resulting time-dependent metric satisfies the Einstein equations with a physically reasonable, time-dependent stress-energy tensor that continues to obey the null energy condition near the would-be singularity as M decreases. This is load-bearing for the self-similarity claim and the applicability of the semiclassical radiation formula used in the DM yield calculation.

    Authors: We agree that a more explicit justification is warranted. In the revised manuscript we have added a derivation in the metric section showing that, under the quasi-static approximation (evaporation timescale ≫ light-crossing time), the instantaneous metric with l(t) = α M(t) yields a stress-energy tensor whose components remain regular and continue to satisfy the null energy condition near the core for both the Hayward and Simpson-Visser cases as M decreases. This supports retention of the standard Hawking temperature formula in the semiclassical regime and bolsters the self-similarity argument. revision: yes

  2. Referee: The allowed parameter space for M_i and l is obtained by requiring the integrated DM yield to equal the observed abundance. This defines the viable region by fitting to the target result rather than producing an independent, falsifiable prediction from the modified temperature and horizon size; the resulting cosmological constraints are therefore weaker than presented.

    Authors: We respectfully disagree. The modified Hawking temperature and horizon radius (functions of both M and l) produce a distinct mass-loss rate dM/dt and DM production spectrum relative to the Schwarzschild case. Integrating these modified rates over the full evaporation history yields a specific relation between M_i and l that reproduces the observed DM density; the resulting allowed region is therefore a genuine, falsifiable prediction of the regular-metric framework rather than an arbitrary fit. We have clarified this distinction and the testability of the bounds in the revised DM-production section. revision: partial

Circularity Check

0 steps flagged

No significant circularity in derivation chain

full rationale

The paper introduces a redefinition of the regularization parameter chosen to preserve self-similarity of evaporation, then computes DM yield from the resulting modified Hawking temperature and horizon radius for Hayward and Simpson-Visser metrics. The final step derives cosmological constraints by requiring the integrated yield to reproduce the observed DM abundance. This is a standard model-to-observation constraint procedure rather than a prediction forced by construction; the yield formula depends on the metric functions and semiclassical radiation, which are independent of the target abundance value. No self-definitional reduction, fitted-input-as-prediction, or load-bearing self-citation chain appears in the abstract or described framework. The derivation remains self-contained against external benchmarks such as the observed DM density.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The framework rests on standard general-relativity assumptions plus the ad-hoc redefinition of the regularization parameter; no new particles or forces are introduced, but the DM abundance is obtained by fitting the initial mass and regularization scale.

free parameters (2)
  • regularization scale l
    Redefined to enforce self-similarity; its value is scanned to match observed DM density.
  • initial PBH mass M_i
    Chosen within a range that yields the correct relic abundance after evaporation.
axioms (2)
  • domain assumption Hawking radiation formula remains valid for the redefined regular metric
    Invoked when computing temperature and evaporation rate for Hayward and Simpson-Visser cases.
  • standard math Standard cosmological expansion history and freeze-out of DM particles
    Used to translate evaporation yield into present-day abundance.

pith-pipeline@v0.9.0 · 5702 in / 1476 out tokens · 37179 ms · 2026-05-22T12:37:31.323282+00:00 · methodology

discussion (0)

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

Forward citations

Cited by 1 Pith paper

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

  1. Memory burden effect of regular primordial black holes

    astro-ph.CO 2026-05 unverdicted novelty 5.0

    Combining regular black hole metrics with memory burden suppresses evaporation and opens a 10^6-10^8 g PBH mass window that can comprise all dark matter.

Reference graph

Works this paper leans on

96 extracted references · 96 canonical work pages · cited by 1 Pith paper · 22 internal anchors

  1. [1]

    self-similarity

    Although the curvature invariants of the Hayward metric are ev erywhere finite, the geodesics are incomplete in this spacetime (at least in the original for m) [25]. This motivates us to also consider another minimal extension of the Schwarzschild s olution which is the Simpson-Visser metric. The curvature invariants of this metric are finite and the geodes...

    work page

  2. [2]

    (23) Even for the smallest PBH mass of order 1 g (see Sec

    75 ) ( g Mi ) 2 . (23) Even for the smallest PBH mass of order 1 g (see Sec. IV), we see th at the formation time is much smaller than the PBH’s lifetime, which is even truer for the RPBH metrics that we 7 Note that A(l) and B(l) are constants for fixed l, so they can be pulled out of the integrals. 9 Hayward Simpson-Visser 0.0 0.5 1.0 1.5 2.0 0.0 0.2 0.4 ...

    work page

  3. [3]

    75 g∗, eva ) 1/ 4 ( g Mi ) 3/ 2

    75 ) 1/ 2 ( 106. 75 g∗, eva ) 1/ 4 ( g Mi ) 3/ 2 . (25) The subscript “eva” denotes the quantities at the evaporation tim e. Next, we calculate the number of emitted particles per BH as: d2Ni dtdE = 4πr 2 H E d2ui dtdE = 2giB(l)2 πm 4 pl M 2E2 eE/T H ± 1 . (26) If the initial Hawking temperature is greater than the particle mass TH,in > m i, where mi is t...

    work page

  4. [4]

    75 g∗, eva ) 1/ 4 ( g∗, i

    75 ) 1/ 2 ( 106. 75 g∗, eva ) 1/ 4 ( g∗, i

    work page

  5. [5]

    0” denotes the values at the present time, the subscript “s

    75 ) 1/ 4 ( g Mi ) , (36) where we used Eqs. 9 and 24. The script “i” denotes values at the fo rmation time of RPBHs. Let χ be a particle DM candidate. Because ρχ ∝ a− 3 and entropy is conserved after RPBH evaporation, the DM abundance today can be calculated as fo llows: Ω χ = ρ0 χ ρ0 crit = 1 ρ0 crit ( aeva a0 ) 3 ρeva χ = 1 ρ0 crit gs, 0T 3 0 gs, evaT ...

    work page

  6. [6]

    Entropy is therefore con served from Ti to Teva, so Eq

    If β < β c: In this case, there is no RPBH domination. Entropy is therefore con served from Ti to Teva, so Eq. 39 becomes: Ω χ = 4π 3 45H 2 0 m2 pl gs, 0T 3 0 TiNχ mχ β Mi . (40) There are two subcases: • If TH,in > m χ , we use Eq. 30 for Nχ and Eq. 9 to obtain: Ω χ ≃ 6. 91 × 108γ1/ 2 1 A(l) gχ ( 106. 75 g∗(TH) ) ( 106. 75 g∗,i ) 1/ 4 ( mχ GeV ) ( Mi g )...

    work page

  7. [7]

    If β ≥ βc: In this case, there is RPBH domination and entropy is not conserved during this period. We instead use the fact that RPBH evaporates when Γ RPBH ∼ Heva to have ρeva RPBH = ρi RPBH ( ai aeva ) 3 (43) = 3m2 plH 2 eva 8π (44) ≃ 3m2 plΓ 2 RPBH 8π (45) = A(l)8B(l)4 3g∗(TH)2m10 pl 8 × (10240)2π 3M 6 i , (46) ⇒ ( ai aeva ) 3 = A(l)8B(l)4 3g∗(TH)2m10 p...

    work page

  8. [8]

    By using Eqs

    19 × 10− 8. By using Eqs. 58, 5, and 24, we obtain an upper bound on RPBH mass : ( Mi g ) ≲ 2. 18 × 105A(l)2B(l)2 ( mχ GeV ) 2 . (60) 0.10 1 10 100 1000m D (G ) 0.01 10 10 107 1010 Mi (g) W ! " d ! # " m m $ ! c % & ' m ! ( & m ) * + - . / 5 6 * + 7 8 9 Hayward, ℓ : ; < Hayward, ℓ : ; = < > ) 7 ? @ 6 A B 7 6 6 / , ℓ C ; E ) 7 ? @ 6 A B 7 6 6 / , ℓ 1.99 FI...

    work page

  9. [9]

    Bardeen Proceedings, 5th International Conference on Gravitation an d the theory of relativity: Tbilisi, USSR, December 9-13, 1968 (1968) p

    J. Bardeen Proceedings, 5th International Conference on Gravitation an d the theory of relativity: Tbilisi, USSR, December 9-13, 1968 (1968) p. 174

    work page 1968

  10. [10]

    Formation and evaporation of non-singular black holes

    S.A. Hayward, Formation and evaporation of regular black holes , Phys. Rev. Lett. 96 (2006) 031103 [ gr-qc/0506126]

    work page internal anchor Pith review Pith/arXiv arXiv 2006

  11. [11]

    Dymnikova, Vacuum nonsingular black hole , Gen

    I. Dymnikova, Vacuum nonsingular black hole , Gen. Rel. Grav. 24 (1992) 235

    work page 1992

  12. [12]

    On a regular modified Schwarzschild spacetime

    H. Culetu, On a regular modified Schwarzschild spacetime , 1305.5964

    work page internal anchor Pith review Pith/arXiv arXiv

  13. [13]

    On a regular charged black hole with a nonlinear electric source

    H. Culetu, On a regular charged black hole with a nonlinear electric sou rce, Int. J. Theor. Phys. 54 (2015) 2855 [ 1408.3334]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  14. [14]

    A nonsingular rotating black hole

    S.G. Ghosh, A nonsingular rotating black hole , Eur. Phys. J. C 75 (2015) 532 [ 1408.5668]. 24

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  15. [15]

    Simpson and M

    A. Simpson and M. Visser, Regular black holes with asymptotically Minkowski cores , Universe 6 (2019) 8 [ 1911.01020]

    work page arXiv 2019

  16. [16]

    Black-bounce to traversable wormhole

    A. Simpson and M. Visser, Black-bounce to traversable wormhole , JCAP 02 (2019) 042 [1812.07114]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  17. [17]

    Complete, Single-Horizon Quantum Corrected Black Hole Spacetime

    A. Peltola and G. Kunstatter, A Complete, Single-Horizon Quantum Corrected Black Hole Spacetime, Phys. Rev. D 79 (2009) 061501 [ 0811.3240]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  18. [18]

    Effective Polymer Dynamics of D-Dimensional Black Hole Interiors

    A. Peltola and G. Kunstatter, Effective Polymer Dynamics of D-Dimensional Black Hole Interiors, Phys. Rev. D 80 (2009) 044031 [ 0902.1746]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  19. [19]

    White Holes as Remnants: A Surprising Scenario for the End of a Black Hole

    E. Bianchi, M. Christodoulou, F. D’Ambrosio, H.M. Hagg ard and C. Rovelli, White Holes as Remnants: A Surprising Scenario for the End of a Black Hole , Class. Quant. Grav. 35 (2018) 225003 [ 1802.04264]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  20. [20]

    How Information Crosses Schwarzschild's Central Singularity

    F. D’Ambrosio and C. Rovelli, How information crosses Schwarzschild’s central singular ity, Class. Quant. Grav. 35 (2018) 215010 [ 1803.05015]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  21. [21]

    C. Lan, H. Yang, Y. Guo and Y.-G. Miao, Regular Black Holes: A Short Topic Review , Int. J. Theor. Phys. 62 (2023) 202 [ 2303.11696]

    work page arXiv 2023

  22. [22]

    Bambi, ed., Regular Black Holes

    C. Bambi, ed., Regular Black Holes. Towards a New Paradigm of Gravitationa l Collapse , Springer Series in Astrophysics and Cosmology, Springer (2 023), 10.1007/978-981-99-1596-5, [2307.13249]

    work page doi:10.1007/978-981-99-1596-5

  23. [23]

    Bambi et al., Black hole mimickers: from theory to observation , 5, 2025 [ 2505.09014]

    C. Bambi et al., Black hole mimickers: from theory to observation , 5, 2025 [ 2505.09014]

    work page arXiv 2025

  24. [24]

    Borissova, S

    J. Borissova, S. Liberati and M. Visser, Violations of the null convergence condition in kinematical transitions between singular and regular blac k holes, horizonless compact objects, and bounces, Phys. Rev. D 111 (2025) 104054 [ 2502.00548]

    work page arXiv 2025

  25. [25]

    Rao and H

    X.-P. Rao and H. Huang, Can we distinguish whether black holes have singularities or not through echoes and light rings? , 2505.11073

    work page arXiv

  26. [26]

    Huang and X.-P

    H. Huang and X.-P. Rao, Regular black holes and their singular families , Phys. Rev. D 111 (2025) 104040 [ 2503.13133]

    work page arXiv 2025

  27. [27]

    Carballo-Rubio, F

    R. Carballo-Rubio, F. Di Filippo, S. Liberati, C. Pacil io and M. Visser, Inner horizon instability and the unstable cores of regular black holes , JHEP 05 (2021) 132 [ 2101.05006]

    work page arXiv 2021

  28. [28]

    Carballo-Rubio, F

    R. Carballo-Rubio, F. Di Filippo, S. Liberati, C. Pacil io and M. Visser, Regular black holes without mass inflation instability , JHEP 09 (2022) 118 [ 2205.13556]

    work page arXiv 2022

  29. [29]

    Cao, L.-Y

    L.-M. Cao, L.-Y. Li, X.-Y. Liu and Y.-S. Zhou, Appearance of the regular black hole with a 25 stable inner horizon , Phys. Rev. D 109 (2024) 064083 [ 2312.04301]

    work page arXiv 2024

  30. [30]

    Bonanno, A.-P

    A. Bonanno, A.-P. Khosravi and F. Saueressig, Regular evaporating black holes with stable cores, Phys. Rev. D 107 (2023) 024005 [ 2209.10612]

    work page arXiv 2023

  31. [31]

    Bonanno and F

    A. Bonanno and F. Saueressig, Stability properties of Regular Black Holes , 2211.09192

    work page arXiv

  32. [32]

    Bonanno, A

    A. Bonanno, A. Panassiti and F. Saueressig, Cauchy Horizon (In)Stability of Regular Black Holes, 2507.03581

    work page arXiv

  33. [33]

    Zhou and L

    T. Zhou and L. Modesto, Geodesic incompleteness of some popular regular black hole s, Phys. Rev. D 107 (2023) 044016 [ 2208.02557]

    work page arXiv 2023

  34. [34]

    Bogdan et al., Evidence for heavy-seed origin of early supermassive black holes from a z ≈ 10 X-ray quasar , Nature Astron

    A. Bogdan et al., Evidence for heavy-seed origin of early supermassive black holes from a z ≈ 10 X-ray quasar , Nature Astron. 8 (2024) 126 [ 2305.15458]

    work page arXiv 2024

  35. [35]

    Kovacs et al., A Candidate Supermassive Black Hole in a Gravitationally Len sed Galaxy at Z ≈ 10, Astrophys

    O.E. Kovacs et al., A Candidate Supermassive Black Hole in a Gravitationally Len sed Galaxy at Z ≈ 10, Astrophys. J. Lett. 965 (2024) L21 [ 2403.14745]

    work page arXiv 2024

  36. [36]

    LIGO Scientific, Virgo collaboration, GW190521: A Binary Black Hole Merger with a Total Mass of 150M⊙ , Phys. Rev. Lett. 125 (2020) 101102 [ 2009.01075]

    work page arXiv 2020

  37. [37]

    LIGO Scientific, VIRGO, KAGRA collaboration, GW231123: a Binary Black Hole Merger with Total Mass 190-265 M⊙ , 2507.08219

    work page internal anchor Pith review Pith/arXiv arXiv

  38. [38]

    et al, Fast-moving stars around an intermediate-mass black hole i n omega centauri , Nature 631, 285-288 (2024)

    M.H. et al, Fast-moving stars around an intermediate-mass black hole i n omega centauri , Nature 631, 285-288 (2024)

    work page 2024

  39. [39]

    Jin et al., An IMBH Lurking in A Galactic Halo Caught Alive during Outburst , 2501.09580

    C.C. Jin et al., An IMBH Lurking in A Galactic Halo Caught Alive during Outburst , 2501.09580

    work page arXiv

  40. [40]

    Cadoni, A.P

    M. Cadoni, A.P. Sanna, M. Pitzalis, B. Banerjee, R. Murg ia, N. Hazra et al., Cosmological coupling of nonsingular black holes , JCAP 11 (2023) 007 [ 2306.11588]

    work page arXiv 2023

  41. [41]

    Cadoni, R

    M. Cadoni, R. Murgia, M. Pitzalis and A.P. Sanna, Quasi-local masses and cosmological coupling of black holes and mimickers , JCAP 03 (2024) 026 [ 2309.16444]

    work page arXiv 2024

  42. [42]

    Farrah et al., Observational Evidence for Cosmological Coupling of Black Ho les and its Implications for an Astrophysical Source of Dark Energy , Astrophys

    D. Farrah et al., Observational Evidence for Cosmological Coupling of Black Ho les and its Implications for an Astrophysical Source of Dark Energy , Astrophys. J. Lett. 944 (2023) L31 [2302.07878]

    work page arXiv 2023

  43. [43]

    Croker, G

    K.S. Croker, G. Tarl´ e, S.P. Ahlen, B.G. Cartwright, D. Farrah, N. Fernandez et al., DESI dark energy time evolution is recovered by cosmologically c oupled black holes , JCAP 10 (2024) 094 [ 2405.12282]

    work page arXiv 2024

  44. [44]

    Faraoni and M

    V. Faraoni and M. Rinaldi, Black hole event horizons are cosmologically coupled , 26 Phys. Rev. D 110 (2024) 063553 [ 2407.14549]

    work page arXiv 2024

  45. [45]

    Calz` a, F

    M. Calz` a, F. Gianesello, M. Rinaldi and S. Vagnozzi, Implications of cosmologically coupled black holes for pulsar timing arrays , Sci. Rep. 14 (2024) 31296 [ 2409.01801]

    work page arXiv 2024

  46. [46]

    Dialektopoulos, T

    K. Dialektopoulos, T. Papanikolaou and V. Zarikas, Primordial black holes as cosmic expansion accelerators, 2502.18352

    work page arXiv

  47. [47]

    Cadoni, M

    M. Cadoni, M. Pitzalis and A.P. Sanna, Apparent horizons in cosmologically-embedded black holes, JCAP 02 (2025) 051 [ 2410.10459]

    work page arXiv 2025

  48. [48]

    Inayoshi, E

    K. Inayoshi, E. Visbal and Z. Haiman, The Assembly of the First Massive Black Holes , Ann. Rev. Astron. Astrophys. 58 (2020) 27 [ 1911.05791]

    work page arXiv 2020

  49. [49]

    Volonteri, M

    M. Volonteri, M. Habouzit and M. Colpi, The origins of massive black holes , Nature Rev. Phys. 3 (2021) 732 [ 2110.10175]

    work page arXiv 2021

  50. [50]

    B.J. Carr, K. Kohri, Y. Sendouda and J. Yokoyama, New cosmological constraints on primordial black holes , Phys. Rev. D 81 (2010) 104019 [ 0912.5297]

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  51. [51]

    Ivanov, P

    P. Ivanov, P. Naselsky and I. Novikov, Inflation and primordial black holes as dark matter , Phys. Rev. D 50 (1994) 7173

    work page 1994

  52. [52]

    Horizon crossing and inflation with large \eta

    W.H. Kinney, Horizon crossing and inflation with large eta , Phys. Rev. D 72 (2005) 023515 [gr-qc/0503017]

    work page internal anchor Pith review Pith/arXiv arXiv 2005

  53. [53]

    Hawking, I.G

    S.W. Hawking, I.G. Moss and J.M. Stewart, Bubble Collisions in the Very Early Universe , Phys. Rev. D 26 (1982) 2681

    work page 1982

  54. [54]

    Black hole formation from colliding bubbles

    I.G. Moss, Black hole formation from colliding bubbles , gr-qc/9405045

    work page internal anchor Pith review Pith/arXiv arXiv

  55. [55]

    Kusenko, M

    A. Kusenko, M. Sasaki, S. Sugiyama, M. Takada, V. Takhis tov and E. Vitagliano, Exploring Primordial Black Holes from the Multiverse with Optical Tel escopes, Phys. Rev. Lett. 125 (2020) 181304 [ 2001.09160]

    work page arXiv 2020

  56. [56]

    Kawana and K.-P

    K. Kawana and K.-P. Xie, Primordial black holes from a cosmic phase transition: The collapse of Fermi-balls , Phys. Lett. B 824 (2022) 136791 [ 2106.00111]

    work page arXiv 2022

  57. [57]

    Penrose, Gravitational collapse and space-time singularities , Phys

    R. Penrose, Gravitational collapse and space-time singularities , Phys. Rev. Lett. 14 (1965) 57

    work page 1965

  58. [58]

    Hawking and R

    S.W. Hawking and R. Penrose, The Singularities of gravitational collapse and cosmology , Proc. Roy. Soc. Lond. A 314 (1970) 529

    work page 1970

  59. [59]

    Hawking and G.F.R

    S.W. Hawking and G.F.R. Ellis, The Large Scale Structure of Space-Time , Cambridge Monographs on Mathematical Physics, Cambridge University Press (2, 2023), 27 10.1017/9781009253161

    work page doi:10.1017/9781009253161 2023

  60. [60]

    Bueno, P.A

    P. Bueno, P.A. Cano and R.A. Hennigar, Regular black holes from pure gravity , Phys. Lett. B 861 (2025) 139260 [ 2403.04827]

    work page arXiv 2025

  61. [61]

    Bueno, P.A

    P. Bueno, P.A. Cano, R.A. Hennigar and A.J. Murcia, Regular black holes from thin-shell collapse, 2412.02740

    work page arXiv

  62. [62]

    Bueno, P.A

    P. Bueno, P.A. Cano, R.A. Hennigar and ´A.J. Murcia, Dynamical Formation of Regular Black Holes , Phys. Rev. Lett. 134 (2025) 181401 [ 2412.02742]

    work page arXiv 2025

  63. [63]

    Bueno, P.A

    P. Bueno, P.A. Cano, R.A. Hennigar and ´A.J. Murcia, Regular black hole formation in four-dimensional non-polynomial gravities , 2509.19016

    work page arXiv

  64. [64]

    Calz` a, D

    M. Calz` a, D. Pedrotti and S. Vagnozzi, Primordial regular black holes as all the dark matter. I. Time-radial-symmetric metrics , Phys. Rev. D 111 (2025) 024009 [ 2409.02804]

    work page arXiv 2025

  65. [65]

    Calz` a, D

    M. Calz` a, D. Pedrotti and S. Vagnozzi, Primordial regular black holes as all the dark matter. II. Non-time-radial-symmetric and loop quantum gravity-ins pired metrics, Phys. Rev. D 111 (2025) 024010 [ 2409.02807]

    work page arXiv 2025

  66. [66]

    Calz` a, D

    M. Calz` a, D. Pedrotti, G.-W. Yuan and S. Vagnozzi, Primordial regular black holes as all the dark matter. III. Covariant canonical quantum gravity models , 2507.02396

    work page arXiv

  67. [67]

    A¸ smano˘ glu, J

    S. A¸ smano˘ glu, J. Boos and C.D. Carone, New models of nonsingular black hole dark matter from limiting curvature , 2507.18322

    work page arXiv

  68. [68]

    Davies, D.A

    P.C.W. Davies, D.A. Easson and P.B. Levin, Nonsingular black holes as dark matter , Phys. Rev. D 111 (2025) 103512 [ 2410.21577]

    work page arXiv 2025

  69. [69]

    Trivedi and A

    O. Trivedi and A. Loeb, Could planck star remnants be dark matter? , Phys. Dark Univ. 49 (2025) 102003 [ 2506.03334]

    work page arXiv 2025

  70. [70]

    Ong, The Case For Black Hole Remnants: A Review , 11, 2024 [ 2412.00322]

    Y.C. Ong, The Case For Black Hole Remnants: A Review , 11, 2024 [ 2412.00322]

    work page arXiv 2024

  71. [71]

    Regular black hole remnants and graviatoms with de Sitter interior as heavy dark matter candidates probing inhomogeneity of early universe

    I. Dymnikova and M. Khlopov, Regular black hole remnants and graviatoms with de Sitter interior as heavy dark matter candidates probing inhomogen eity of early universe , Int. J. Mod. Phys. D 24 (2015) 1545002 [ 1510.01351]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  72. [72]

    Kumar, D.V

    A. Kumar, D.V. Singh and S.G. Ghosh, Hayward black holes in Einstein–Gauss–Bonnet gravity, Annals Phys. 419 (2020) 168214 [ 2003.14016]

    work page arXiv 2020

  73. [73]

    Addazi et al

    A. Addazi et al., Quantum gravity phenomenology at the dawn of the multi-mess enger era—A review , Prog. Part. Nucl. Phys. 125 (2022) 103948 [ 2111.05659]

    work page arXiv 2022

  74. [74]

    Bronnikov and R.K

    K.A. Bronnikov and R.K. Walia, Field sources for Simpson-Visser spacetimes , 28 Phys. Rev. D 105 (2022) 044039 [ 2112.13198]

    work page arXiv 2022

  75. [75]

    Hawking, Black hole explosions , Nature 248 (1974) 30

    S.W. Hawking, Black hole explosions , Nature 248 (1974) 30

    work page 1974

  76. [76]

    Hawking, Particle Creation by Black Holes , Commun

    S.W. Hawking, Particle Creation by Black Holes , Commun. Math. Phys. 43 (1975) 199

    work page 1975

  77. [77]

    Gibbons and S.W

    G.W. Gibbons and S.W. Hawking, Cosmological Event Horizons, Thermodynamics, and Particle Creation, Phys. Rev. D 15 (1977) 2738

    work page 1977

  78. [78]

    Bolokhov and R.A

    S.V. Bolokhov and R.A. Konoplya, Circumventing quantum gravity: Black holes evaporating into macroscopic wormholes , Phys. Rev. D 111 (2025) 064007 [ 2410.10419]

    work page arXiv 2025

  79. [79]

    Khodadi, Could regular primordial black holes be dark matter? , Phys

    M. Khodadi, Could regular primordial black holes be dark matter? , Phys. Lett. B 870 (2025) 139922 [ 2509.20483]

    work page arXiv 2025

  80. [80]

    Carr, The Primordial black hole mass spectrum , Astrophys

    B.J. Carr, The Primordial black hole mass spectrum , Astrophys. J. 201 (1975) 1

    work page 1975

Showing first 80 references.