pith. machine review for the scientific record. sign in

arxiv: 2601.19386 · v2 · submitted 2026-01-27 · ✦ hep-ph · astro-ph.HE

Recognition: no theorem link

Constraints on Primordial Black Holes from Galactic Diffuse Synchrotron Emissions

Chen-Wei Du , Yu-Feng Zhou
Authors on Pith no claims yet

Pith reviewed 2026-05-16 10:54 UTC · model grok-4.3

classification ✦ hep-ph astro-ph.HE
keywords primordial black holesHawking radiationsynchrotron emissioncosmic ray propagationdiffusive re-accelerationGalactic diffuse emissionselectron positron constraints
0
0 comments X

The pith

Low-frequency synchrotron emissions constrain primordial black hole abundance more tightly than Voyager-1 data for masses above 10^16 grams.

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

The paper examines how Hawking radiation from primordial black holes with masses above 10^15 grams produces low-energy electrons and positrons that, in certain cosmic-ray propagation models, get re-accelerated to energies around 100 MeV. These particles then generate detectable synchrotron radiation in the Galaxy's magnetic fields at frequencies from 22 MHz upward. Using benchmark models where the Alfvén velocity is around 20 km/s, confirmed by boron-to-carbon ratio data, the observed diffuse synchrotron background yields abundance limits on these black holes. The resulting bounds exceed those from direct Voyager-1 electron measurements by more than an order of magnitude for masses greater than or equal to 10^16 grams.

Core claim

In diffusive re-acceleration models with Alfvén velocity Va approximately 20 km/s, the Galactic synchrotron emissions observed between 22 MHz and 1.4 GHz impose conservative upper limits on the PBH dark-matter fraction that are stronger than Voyager-1 all-electron constraints by over one order of magnitude for M_PBH greater than or equal to 1 times 10^16 g, and stronger than prior AMS-02 positron-based limits for M_PBH greater than or equal to 2 times 10^16 g.

What carries the argument

Diffusive re-acceleration of PBH-evaporated electrons and positrons by Galactic magnetic turbulence, parameterized by a single Alfvén velocity Va ~ 20 km/s that boosts their energies from below 10 MeV to O(100) MeV and thereby produces observable synchrotron radiation.

If this is right

  • For M_PBH around 10^16 g, the synchrotron limits become the strongest existing constraint from indirect searches.
  • The method extends to slightly higher masses up to roughly 10^17 g before the injected electrons fall below the re-acceleration threshold.
  • Future radio surveys with better foreground subtraction could improve the bounds by another factor of a few.
  • The same re-acceleration framework links PBH signals to existing fits of nuclear secondary ratios, reducing model freedom.

Where Pith is reading between the lines

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

  • If the Alfvén velocity varies spatially, the synchrotron signal might concentrate in regions of stronger turbulence, offering a spatial signature to test against uniform PBH distributions.
  • The approach could be combined with future MeV gamma-ray telescopes to cross-check the same electron population through inverse-Compton emission.
  • A detection of excess low-frequency synchrotron correlated with Galactic center or halo morphology would favor a PBH origin over conventional astrophysical sources.

Load-bearing premise

That the same diffusive re-acceleration model fitted to nuclear cosmic rays also governs the propagation and energy gains of the lower-energy electrons and positrons from PBHs, with no large extra synchrotron contributions from unrelated sources.

What would settle it

A measured synchrotron intensity at 22-408 MHz significantly lower than the excess predicted for a PBH abundance at the current upper limit, or a boron-to-carbon ratio that forces Va below 10 km/s in the same propagation setup.

Figures

Figures reproduced from arXiv: 2601.19386 by Chen-Wei Du, Yu-Feng Zhou.

Figure 1
Figure 1. Figure 1: FIG. 1. Model predictions and residuals of B/C flux ratio for the benchmark models. Left: for [PITH_FULL_IMAGE:figures/full_fig_p013_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2. The LIS energy spectra of evaporated all-electrons at the Solar position for CR propagation [PITH_FULL_IMAGE:figures/full_fig_p015_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3. Sky maps of synchrotron signals of PBHs with NFW and Burkert DM profiles (left and [PITH_FULL_IMAGE:figures/full_fig_p022_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4. Same as Fig [PITH_FULL_IMAGE:figures/full_fig_p023_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5. Spectra of synchrotron signals of PBHs for GH, DRz4, DRz6 and DBz4 CR propagation [PITH_FULL_IMAGE:figures/full_fig_p024_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6. Constraints on [PITH_FULL_IMAGE:figures/full_fig_p026_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: FIG. 7. Constraints on [PITH_FULL_IMAGE:figures/full_fig_p027_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: FIG. 8. The first seven: ratio of synchrotron signals to observational limits (intensity + 2 [PITH_FULL_IMAGE:figures/full_fig_p028_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: FIG. 9. Same as Fig [PITH_FULL_IMAGE:figures/full_fig_p029_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: FIG. 10. Constraints on [PITH_FULL_IMAGE:figures/full_fig_p030_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: FIG. 11. Several constraints on [PITH_FULL_IMAGE:figures/full_fig_p031_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: FIG. 12. Model predictions and residuals of C flux for the benchmark models. Left: for Voyager-1. [PITH_FULL_IMAGE:figures/full_fig_p047_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: FIG. 13. Corner plots of posterior PDFs for DRz4, DRz6, and DRz10 models. The result of [PITH_FULL_IMAGE:figures/full_fig_p048_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: FIG. 14. Constraints on [PITH_FULL_IMAGE:figures/full_fig_p049_14.png] view at source ↗
Figure 15
Figure 15. Figure 15: FIG. 15. Constraints on [PITH_FULL_IMAGE:figures/full_fig_p050_15.png] view at source ↗
Figure 16
Figure 16. Figure 16: FIG. 16. Same as Fig [PITH_FULL_IMAGE:figures/full_fig_p051_16.png] view at source ↗
Figure 17
Figure 17. Figure 17: FIG. 17. Same as Fig [PITH_FULL_IMAGE:figures/full_fig_p051_17.png] view at source ↗
read the original abstract

We investigate the possibility of constraining primordial black holes (PBHs) with masses $M_\mathrm{PBH}\gtrsim 10^{15}\,\mathrm{g}$ through Galactic diffuse synchrotron emissions. Due to Hawking radiation, these types of PBHs are expected to be stable sources of cosmic-ray (CR) electrons and positrons with energies below $\mathcal{O}(10\,\mathrm{MeV})$. In many CR propagation models with diffusive re-acceleration characterized by a significant Alfv\'{e}n velocity $V_a\sim \mathcal{O}(10)\,\mathrm{km/s}$, the energies of the evaporated electrons/positrons can be further enhanced to $\mathcal{O}(100)\,\mathrm{MeV}$ through their scattering with the Galactic random magnetic fields. Consequently, the observation of Galactic synchrotron emissions at frequencies above $\sim 20\,\mathrm{MHz}$ can provide useful constraints on the abundance of PBHs. Using the AMS-02 and Voyager-1 data on the boron-to-carbon nuclei flux ratio, we confirm that a significant Alfv\'{e}n velocity $V_a \sim 20\,\mathrm{km/s}$ is favored in several benchmark diffusive re-acceleration models. We show that, in this scenario, the observed low-frequency synchrotron emissions (from 22 MHz to 1.4 GHz) can provide stringent constraints on PBH abundance. The obtained conservative constraints are stronger than those derived from the Voyager-1 all-electron (electron plus positron) data by more than one order of magnitude for $M_\mathrm{PBH}\gtrsim 1\times 10^{16}\,\mathrm{g}$, and also stronger than our previous constraints derived from the AMS-02 positron data for $M_\mathrm{PBH}\gtrsim 2\times 10^{16}\,\mathrm{g}$.

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 / 1 minor

Summary. The manuscript investigates constraints on primordial black holes (PBHs) with masses M_PBH ≳ 10^15 g using Galactic diffuse synchrotron emissions. Hawking radiation from these PBHs produces electrons and positrons below O(10 MeV); in diffusive re-acceleration models with Alfvén velocity Va ~ 20 km/s (calibrated to AMS-02 and Voyager-1 boron-to-carbon ratios), these particles are boosted to O(100 MeV) and generate synchrotron radiation observable at frequencies from 22 MHz to 1.4 GHz. The paper claims that the observed low-frequency synchrotron flux yields PBH abundance limits stronger than Voyager-1 all-electron data by more than an order of magnitude for M_PBH ≥ 10^16 g and stronger than prior AMS-02 positron constraints for M_PBH ≳ 2×10^16 g.

Significance. If the propagation assumptions hold, the result supplies a new, independent probe of PBH dark-matter candidates that leverages existing radio data and standard cosmic-ray frameworks. It demonstrates how re-acceleration can convert a low-energy Hawking signal into a detectable synchrotron signature, tightening bounds relative to direct lepton measurements and offering a falsifiable prediction tied to the fitted Va value.

major comments (2)
  1. [Propagation modeling and Va calibration] The transfer of the single-Va diffusive re-acceleration model (D_pp ∝ Va²) from nuclear B/C data to PBH-injected electrons/positrons at E ≲ 10 MeV is load-bearing for the central claim. At these energies ionization and Coulomb losses dominate for leptons, unlike the rigidity-dependent losses relevant for nuclei; this difference can modify the equilibrium spectrum of the ~50–200 MeV leptons responsible for the 20 MHz–1.4 GHz synchrotron signal. A dedicated propagation run or analytic estimate showing that the boost to O(100 MeV) remains robust under lepton-specific losses is required.
  2. [Synchrotron flux comparison and limit derivation] The synchrotron limits treat the full observed flux (22 MHz–1.4 GHz) as an upper bound on the PBH contribution. No quantitative subtraction or upper limit is provided for other Galactic synchrotron sources (secondary electrons from hadronic interactions, discrete sources). Any non-negligible background would directly weaken the reported >10× improvement over Voyager-1 constraints.
minor comments (1)
  1. [Abstract] The abstract states the constraints are 'stronger … by more than one order of magnitude'; quoting the precise numerical factor (or range) obtained for each mass bin would improve clarity.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the careful and constructive review of our manuscript. We address each major comment in detail below, providing the strongest honest defense of our approach while incorporating revisions where they improve clarity or robustness.

read point-by-point responses

  1. Referee: [Propagation modeling and Va calibration] The transfer of the single-Va diffusive re-acceleration model (D_pp ∝ Va²) from nuclear B/C data to PBH-injected electrons/positrons at E ≲ 10 MeV is load-bearing for the central claim. At these energies ionization and Coulomb losses dominate for leptons, unlike the rigidity-dependent losses relevant for nuclei; this difference can modify the equilibrium spectrum of the ~50–200 MeV leptons responsible for the 20 MHz–1.4 GHz synchrotron signal. A dedicated propagation run or analytic estimate showing that the boost to O(100 MeV) remains robust under lepton-specific losses is required.

    Authors: We thank the referee for this important observation on lepton propagation. Our Va calibration follows the standard practice of using nuclear B/C data (AMS-02 and Voyager-1) to fix the re-acceleration strength in benchmark models such as those implemented in GALPROP. To directly address the distinct loss processes for leptons, we have added an analytic estimate (new Appendix A in the revised manuscript) that solves the steady-state transport equation including ionization, Coulomb, and synchrotron losses together with the re-acceleration term D_pp ∝ Va². The calculation shows that particles injected below 10 MeV are still re-accelerated into the 50–200 MeV window on timescales shorter than the dominant loss times at those energies, preserving the O(100 MeV) boost needed for the synchrotron signal. While a full numerical propagation run with lepton-specific losses would be desirable, the analytic result demonstrates that the central claim remains robust; we have therefore revised Section 3 to include this estimate and the associated discussion. revision: yes

  2. Referee: [Synchrotron flux comparison and limit derivation] The synchrotron limits treat the full observed flux (22 MHz–1.4 GHz) as an upper bound on the PBH contribution. No quantitative subtraction or upper limit is provided for other Galactic synchrotron sources (secondary electrons from hadronic interactions, discrete sources). Any non-negligible background would directly weaken the reported >10× improvement over Voyager-1 constraints.

    Authors: The referee correctly identifies that the measured synchrotron intensity contains contributions from secondary electrons, discrete sources, and other processes. Our limits are derived by conservatively assigning the entire observed flux to the PBH component; this choice deliberately avoids reliance on uncertain background models and yields robust upper bounds on the PBH abundance. We have revised the text in Section 4 and the conclusions to state this conservative philosophy explicitly and to note that any future subtraction of non-PBH contributions would only tighten the constraints further. Because the reported improvement over Voyager-1 is already obtained under this conservative assumption, the >10× factor remains a valid lower bound on the improvement; we therefore do not perform a quantitative background subtraction at this stage. revision: partial

Circularity Check

0 steps flagged

Minor self-citation for comparison only; central constraints derived from independent synchrotron observations

full rationale

The derivation fits the Alfvén velocity Va ≈ 20 km/s from boron-to-carbon ratio data in the diffusive re-acceleration model. This parameter is then used in the same propagation framework to compute the synchrotron emission from electrons/positrons injected by PBHs. The resulting flux is compared against observed Galactic diffuse synchrotron data (22 MHz to 1.4 GHz) to derive upper limits on PBH abundance. This process does not reduce to the input by construction because the synchrotron measurements constitute an independent dataset. The paper references prior constraints from the same authors using AMS-02 positron data solely for comparative purposes, without relying on them to establish the new limits. No self-definitional loops, fitted inputs renamed as predictions, or ansatz smuggling via self-citation are present. The central claim remains supported by the application of the model to a new observable.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The analysis relies on one fitted propagation parameter and standard assumptions about Hawking radiation and Galactic transport; no new particles or forces are introduced.

free parameters (1)
  • Alfvén velocity Va = 20 km/s
    Fitted to AMS-02 and Voyager-1 boron-to-carbon ratio data within diffusive re-acceleration models; value approximately 20 km/s is adopted for the synchrotron calculation.
axioms (2)
  • domain assumption Standard diffusive re-acceleration model governs cosmic-ray transport in the Galaxy
    Invoked to relate the boron-to-carbon ratio to the Alfvén velocity and to propagate black-hole-injected electrons and positrons.
  • standard math Hawking radiation from primordial black holes produces electrons and positrons below O(10 MeV)
    Standard result from quantum field theory in curved spacetime, used without re-derivation.

pith-pipeline@v0.9.0 · 5628 in / 1552 out tokens · 30796 ms · 2026-05-16T10:54:46.644906+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

172 extracted references · 172 canonical work pages · 85 internal anchors

  1. [1]

    Particle Dark Matter: Evidence, Candidates and Constraints

    G. Bertone, D. Hooper, and J. Silk, “Particle dark matter: Evidence, candidates and constraints,”Phys. Rept.405(2005) 279–390,arXiv:hep-ph/0404175

    work page internal anchor Pith review Pith/arXiv arXiv 2005

  2. [2]

    TASI Lectures on Indirect Detection of Dark Matter

    T. R. Slatyer, “Indirect detection of dark matter.,” inTheoretical Advanced Study Institute in Elementary Particle Physics: Anticipating the Next Discoveries in Particle Physics, pp. 297–353. 2018.arXiv:1710.05137 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  3. [3]

    TASI lectures on dark matter models and direct detection

    T. Lin, “Dark matter models and direct detection,”PoS333(2019) 009, arXiv:1904.07915 [hep-ph]. 32

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  4. [4]

    Gravitationally collapsed objects of very low mass,

    S. Hawking, “Gravitationally collapsed objects of very low mass,”Mon. Not. Roy. Astron. Soc.152(1971) 75

    work page 1971

  5. [5]

    Black holes in the early Universe,

    B. J. Carr and S. W. Hawking, “Black holes in the early Universe,”Mon. Not. Roy. Astron. Soc.168(1974) 399–415

    work page 1974

  6. [6]

    Cosmological effects of primordial black holes,

    G. F. Chapline, “Cosmological effects of primordial black holes,”Nature253no. 5489, (1975) 251–252

    work page 1975

  7. [7]

    Primeval black holes and galaxy formation,

    P. Meszaros, “Primeval black holes and galaxy formation,”Astron. Astrophys.38(1975) 5–13

    work page 1975

  8. [8]

    The Primordial black hole mass spectrum,

    B. J. Carr, “The Primordial black hole mass spectrum,”Astrophys. J.201(1975) 1–19

    work page 1975

  9. [9]

    Constraints on Primordial Black Holes by Distortions of Cosmic Microwave Background

    H. Tashiro and N. Sugiyama, “Constraints on Primordial Black Holes by Distortions of Cosmic Microwave Background,”Phys. Rev. D78(2008) 023004,arXiv:0801.3172 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  10. [10]

    The abundance of primordial black holes depends on the shape of the inflationary power spectrum

    C. Germani and I. Musco, “Abundance of Primordial Black Holes Depends on the Shape of the Inflationary Power Spectrum,”Phys. Rev. Lett.122no. 14, (2019) 141302, arXiv:1805.04087 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  11. [11]

    Single Field Double Inflation and Primordial Black Holes

    K. Kannike, L. Marzola, M. Raidal, and H. Veerm¨ ae, “Single Field Double Inflation and Primordial Black Holes,”JCAP09(2017) 020,arXiv:1705.06225 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  12. [12]

    Primordial black hole constraints for extended mass functions

    B. Carr, M. Raidal, T. Tenkanen, V. Vaskonen, and H. Veerm¨ ae, “Primordial black hole constraints for extended mass functions,”Phys. Rev. D96no. 2, (2017) 023514, arXiv:1705.05567 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  13. [13]

    Primordial black holes from inflaton and spectator field perturbations in a matter-dominated era

    B. Carr, T. Tenkanen, and V. Vaskonen, “Primordial black holes from inflaton and spectator field perturbations in a matter-dominated era,”Phys. Rev. D96no. 6, (2017) 063507,arXiv:1706.03746 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  14. [14]

    Spontaneous Generation of Density Perturbations in the Early Universe,

    M. Crawford and D. N. Schramm, “Spontaneous Generation of Density Perturbations in the Early Universe,”Nature298(1982) 538–540

    work page 1982

  15. [15]

    Bubble Collisions in the Very Early Universe,

    S. W. Hawking, I. G. Moss, and J. M. Stewart, “Bubble Collisions in the Very Early Universe,”Phys. Rev. D26(1982) 2681

    work page 1982

  16. [16]

    Primordial black holes with an accurate QCD equation of state

    C. T. Byrnes, M. Hindmarsh, S. Young, and M. R. S. Hawkins, “Primordial black holes with an accurate QCD equation of state,”JCAP08(2018) 041,arXiv:1801.06138 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  17. [17]

    Primordial Black Holes from QCD Axion Bubbles,

    N. Kitajima and F. Takahashi, “Primordial Black Holes from QCD Axion Bubbles,”JCAP 11(2020) 060,arXiv:2006.13137 [hep-ph]

    work page arXiv 2020

  18. [18]

    Primordial black holes from confinement,

    G. Dvali, F. K¨ uhnel, and M. Zantedeschi, “Primordial black holes from confinement,”Phys. Rev. D104no. 12, (2021) 123507,arXiv:2108.09471 [hep-ph]

    work page arXiv 2021

  19. [19]

    Constraints on Primordial Black Holes

    B. Carr, K. Kohri, Y. Sendouda, and J. Yokoyama, “Constraints on primordial black holes,”Rept. Prog. Phys.84no. 11, (2021) 116902,arXiv:2002.12778 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2021

  20. [20]

    Primordial black holes as dark matter candidates,

    B. Carr and F. Kuhnel, “Primordial black holes as dark matter candidates,”SciPost Phys. Lect. Notes48(2022) 1,arXiv:2110.02821 [astro-ph.CO]. 33

    work page arXiv 2022

  21. [21]

    Primordial black hole constraints with Hawking radiation—A review,

    J. Auffinger, “Primordial black hole constraints with Hawking radiation—A review,”Prog. Part. Nucl. Phys.131(2023) 104040,arXiv:2206.02672 [astro-ph.CO]. [23]MACHOCollaboration, C. Alcocket al., “The MACHO project: Microlensing results from 5.7 years of LMC observations,”Astrophys. J.542(2000) 281–307, arXiv:astro-ph/0001272. [24]MachoCollaboration, R. A....

    work page arXiv 2023

  22. [22]

    The OGLE View of Microlensing towards the Magellanic Clouds. III. Ruling out sub-solar MACHOs with the OGLE-III LMC data

    L. Wyrzykowskiet al., “The OGLE View of Microlensing towards the Magellanic Clouds. III. Ruling out sub-solar MACHOs with the OGLE-III LMC data,”Mon. Not. Roy. Astron. Soc.413(2011) 493,arXiv:1012.1154 [astro-ph.GA]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  23. [23]

    The OGLE View of Microlensing towards the Magellanic Clouds. IV. OGLE-III SMC Data and Final Conclusions on MACHOs

    L. Wyrzykowskiet al., “The OGLE View of Microlensing towards the Magellanic Clouds. IV. OGLE-III SMC Data and Final Conclusions on MACHOs,”Mon. Not. Roy. Astron. Soc.416(2011) 2949,arXiv:1106.2925 [astro-ph.GA]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  24. [24]

    Experimental Limits on Primordial Black Hole Dark Matter from the First Two Years of Kepler Data

    K. Griest, A. M. Cieplak, and M. J. Lehner, “Experimental Limits on Primordial Black Hole Dark Matter from the First 2 yr of Kepler Data,”Astrophys. J.786no. 2, (2014) 158, arXiv:1307.5798 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  25. [25]

    Microlensing towards the SMC: a new analysis of OGLE and EROS results

    S. Calchi Novati, S. Mirzoyan, P. Jetzer, and G. Scarpetta, “Microlensing towards the SMC: a new analysis of OGLE and EROS results,”Mon. Not. Roy. Astron. Soc.435 (2013) 1582,arXiv:1308.4281 [astro-ph.GA]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  26. [26]

    New limits on primordial black hole dark matter from an analysis of kepler source microlensing data,

    K. Griest, A. M. Cieplak, and M. J. Lehner, “New limits on primordial black hole dark matter from an analysis of kepler source microlensing data,”Phys. Rev. Lett.111(Oct,

    work page

  27. [27]

    181302.https://link.aps.org/doi/10.1103/PhysRevLett.111.181302

    work page doi:10.1103/physrevlett.111.181302

  28. [28]

    Gravitational Waves from Primordial Black Hole Mergers

    M. Raidal, V. Vaskonen, and H. Veerm¨ ae, “Gravitational Waves from Primordial Black Hole Mergers,”JCAP09(2017) 037,arXiv:1707.01480 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  29. [29]

    Formation and Evolution of Primordial Black Hole Binaries in the Early Universe

    M. Raidal, C. Spethmann, V. Vaskonen, and H. Veerm¨ ae, “Formation and Evolution of Primordial Black Hole Binaries in the Early Universe,”JCAP02(2019) 018, arXiv:1812.01930 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  30. [30]

    Lower bound on the primordial black hole merger rate,

    V. Vaskonen and H. Veerm¨ ae, “Lower bound on the primordial black hole merger rate,” Phys. Rev. D101no. 4, (2020) 043015,arXiv:1908.09752 [astro-ph.CO]

    work page arXiv 2020

  31. [31]

    Pulsar Timing Array Constraints on Primordial Black Holes with NANOGrav 11-Year Data Set,

    Z.-C. Chen, C. Yuan, and Q.-G. Huang, “Pulsar Timing Array Constraints on Primordial Black Holes with NANOGrav 11-Year Dataset,”Phys. Rev. Lett.124no. 25, (2020) 25, arXiv:1910.12239 [astro-ph.CO]

    work page arXiv 2020

  32. [32]

    Gravitational wave background as a probe of the primordial black hole abundance

    R. Saito and J. Yokoyama, “Gravitational wave background as a probe of the primordial black hole abundance,”Phys. Rev. Lett.102(2009) 161101,arXiv:0812.4339 [astro-ph]. [Erratum: Phys.Rev.Lett. 107, 069901 (2011)]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  33. [33]

    Constraints on primordial density perturbations from induced gravitational waves

    H. Assadullahi and D. Wands, “Constraints on primordial density perturbations from induced gravitational waves,”Phys. Rev. D81(2010) 023527,arXiv:0907.4073 34 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  34. [34]

    Constraints on the induced gravitational wave background from primordial black holes

    E. Bugaev and P. Klimai, “Constraints on the induced gravitational wave background from primordial black holes,”Phys. Rev. D83(2011) 083521,arXiv:1012.4697 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  35. [35]

    Dynamical constraints on dark compact objects,

    B. J. Carr and M. Sakellariadou, “Dynamical constraints on dark compact objects,” Astrophys. J.516(1999) 195–220

    work page 1999

  36. [36]

    The end of the MACHO era- revisited: new limits on MACHO masses from halo wide binaries

    M. A. Monroy-Rodr´ ıguez and C. Allen, “The end of the MACHO era- revisited: new limits on MACHO masses from halo wide binaries,”Astrophys. J.790no. 2, (2014) 159, arXiv:1406.5169 [astro-ph.GA]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  37. [37]

    Constraints on MACHO Dark Matter from Compact Stellar Systems in Ultra-Faint Dwarf Galaxies

    T. D. Brandt, “Constraints on MACHO Dark Matter from Compact Stellar Systems in Ultra-Faint Dwarf Galaxies,”Astrophys. J. Lett.824no. 2, (2016) L31,arXiv:1605.03665 [astro-ph.GA]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  38. [38]

    Dynamics of dwarf galaxies disfavor stellar-mass black hole dark matter

    S. M. Koushiappas and A. Loeb, “Dynamics of Dwarf Galaxies Disfavor Stellar-Mass Black Holes as Dark Matter,”Phys. Rev. Lett.119no. 4, (2017) 041102,arXiv:1704.01668 [astro-ph.GA]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  39. [39]

    Primordial Black Holes as Generators of Cosmic Structures

    B. Carr and J. Silk, “Primordial Black Holes as Generators of Cosmic Structures,”Mon. Not. Roy. Astron. Soc.478no. 3, (2018) 3756–3775,arXiv:1801.00672 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  40. [40]

    Black hole explosions,

    S. W. Hawking, “Black hole explosions,”Nature248(1974) 30–31

    work page 1974

  41. [41]

    Particle Creation by Black Holes,

    S. W. Hawking, “Particle Creation by Black Holes,”Commun. Math. Phys.43(1975) 199–220. [Erratum: Commun.Math.Phys. 46, 206 (1976)]

    work page 1975

  42. [42]

    Baldes, Q

    I. Baldes, Q. Decant, D. C. Hooper, and L. Lopez-Honorez, “Non-Cold Dark Matter from Primordial Black Hole Evaporation,”JCAP08(2020) 045,arXiv:2004.14773 [astro-ph.CO]

    work page arXiv 2020

  43. [43]

    Cheek, L

    A. Cheek, L. Heurtier, Y. F. Perez-Gonzalez, and J. Turner, “Primordial black hole evaporation and dark matter production. I. Solely Hawking radiation,”Phys. Rev. D105 no. 1, (2022) 015022,arXiv:2107.00013 [hep-ph]

    work page arXiv 2022

  44. [44]

    Quark and gluon jet emission from primordial black holes. 2. The Lifetime emission,

    J. H. MacGibbon, “Quark and gluon jet emission from primordial black holes. 2. The Lifetime emission,”Phys. Rev. D44(1991) 376–392

    work page 1991

  45. [45]

    New cosmological constraints on primordial black holes

    B. J. Carr, K. Kohri, Y. Sendouda, and J. Yokoyama, “New cosmological constraints on primordial black holes,”Phys. Rev. D81(2010) 104019,arXiv:0912.5297 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  46. [46]

    Constraints on primordial black holes from Galactic gamma-ray background

    B. J. Carr, K. Kohri, Y. Sendouda, and J. Yokoyama, “Constraints on primordial black holes from the Galactic gamma-ray background,”Phys. Rev. D94no. 4, (2016) 044029, arXiv:1604.05349 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  47. [47]

    Constraining primordial black hole masses with the isotropic gamma ray background,

    A. Arbey, J. Auffinger, and J. Silk, “Constraining primordial black hole masses with the isotropic gamma ray background,”Phys. Rev. D101no. 2, (2020) 023010, arXiv:1906.04750 [astro-ph.CO]

    work page arXiv 2020

  48. [48]

    INTEGRAL constraints on primordial black holes and particle dark matter,

    R. Laha, J. B. Mu˜ noz, and T. R. Slatyer, “INTEGRAL constraints on primordial black 35 holes and particle dark matter,”Phys. Rev. D101no. 12, (2020) 123514, arXiv:2004.00627 [astro-ph.CO]

    work page arXiv 2020

  49. [49]

    Neutrino and positron constraints on spinning primordial black hole dark matter,

    B. Dasgupta, R. Laha, and A. Ray, “Neutrino and positron constraints on spinning primordial black hole dark matter,”Phys. Rev. Lett.125no. 10, (2020) 101101, arXiv:1912.01014 [hep-ph]

    work page arXiv 2020

  50. [50]

    Primordial Black Holes as a Dark Matter Candidate Are Severely Constrained by the Galactic Center 511 keV γ -Ray Line,

    R. Laha, “Primordial Black Holes as a Dark Matter Candidate Are Severely Constrained by the Galactic Center 511 keVγ-Ray Line,”Phys. Rev. Lett.123no. 25, (2019) 251101, arXiv:1906.09994 [astro-ph.HE]

    work page arXiv 2019

  51. [51]

    511 keV excess and primordial black holes,

    C. Keith and D. Hooper, “511 keV excess and primordial black holes,”Phys. Rev. D104 no. 6, (2021) 063033,arXiv:2103.08611 [astro-ph.CO]

    work page arXiv 2021

  52. [52]

    Refining Galactic primordial black hole evaporation constraints,

    P. De la Torre Luque, J. Koechler, and S. Balaji, “Refining Galactic primordial black hole evaporation constraints,”Phys. Rev. D110no. 12, (2024) 123022,arXiv:2406.11949 [astro-ph.HE]

    work page arXiv 2024

  53. [53]

    Planck Constraint on Relic Primordial Black Holes

    S. Clark, B. Dutta, Y. Gao, L. E. Strigari, and S. Watson, “Planck Constraint on Relic Primordial Black Holes,”Phys. Rev. D95no. 8, (2017) 083006,arXiv:1612.07738 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  54. [54]

    CMB and BBN constraints on evaporating primordial black holes revisited,

    S. K. Acharya and R. Khatri, “CMB and BBN constraints on evaporating primordial black holes revisited,”JCAP06(2020) 018,arXiv:2002.00898 [astro-ph.CO]

    work page arXiv 2020

  55. [55]

    Constraining primordial black holes as dark matter using the global 21-cm signal with X-ray heating and excess radio background,

    S. Mittal, A. Ray, G. Kulkarni, and B. Dasgupta, “Constraining primordial black holes as dark matter using the global 21-cm signal with X-ray heating and excess radio background,”JCAP03(2022) 030,arXiv:2107.02190 [astro-ph.CO]

    work page arXiv 2022

  56. [56]

    Constraining primordial black holes as dark matter at JUNO,

    S. Wang, D.-M. Xia, X. Zhang, S. Zhou, and Z. Chang, “Constraining primordial black holes as dark matter at JUNO,”Phys. Rev. D103no. 4, (2021) 043010, arXiv:2010.16053 [hep-ph]

    work page arXiv 2021

  57. [57]

    Current and future neutrino limits on the abundance of primordial black holes,

    N. Bernal, V. Mu˜ noz-Albornoz, S. Palomares-Ruiz, and P. Villanueva-Domingo, “Current and future neutrino limits on the abundance of primordial black holes,”JCAP10(2022) 068,arXiv:2203.14979 [hep-ph]

    work page arXiv 2022

  58. [58]

    Sensitivity floor for primordial black holes in neutrino searches,

    Q. Liu and K. C. Y. Ng, “Sensitivity floor for primordial black holes in neutrino searches,” Phys. Rev. D110no. 6, (2024) 063024,arXiv:2312.06108 [hep-ph]

    work page arXiv 2024

  59. [59]

    Voyager 1 $e^\pm$ Further Constrain Primordial Black Holes as Dark Matter

    M. Boudaud and M. Cirelli, “Voyager 1e ± Further Constrain Primordial Black Holes as Dark Matter,”Phys. Rev. Lett.122no. 4, (2019) 041104,arXiv:1807.03075 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  60. [60]

    Constraints on evaporating primordial black holes from the AMS-02 positron data,

    J.-Z. Huang and Y.-F. Zhou, “Constraints on evaporating primordial black holes from the AMS-02 positron data,”Phys. Rev. D111no. 8, (2025) 083525,arXiv:2403.04987 [hep-ph]

    work page arXiv 2025

  61. [61]

    Local Flux of Low-Energy Antiprotons from Evaporating Primordial Black Holes

    K. Maki, T. Mitsui, and S. Orito, “Local flux of low-energy anti-protons from evaporating primordial black holes,”Phys. Rev. Lett.76(1996) 3474–3477,arXiv:astro-ph/9601025

    work page internal anchor Pith review Pith/arXiv arXiv 1996

  62. [62]

    Antiprotons from primordial black holes

    A. Barrau, G. Boudoul, F. Donato, D. Maurin, P. Salati, and R. Taillet, “Anti-protons from 36 primordial black holes,”Astron. Astrophys.388(2002) 676,arXiv:astro-ph/0112486

    work page internal anchor Pith review Pith/arXiv arXiv 2002

  63. [63]

    Constraints on cosmic-ray propagation models from a global Bayesian analysis

    R. Trotta, G. J´ ohannesson, I. V. Moskalenko, T. A. Porter, R. R. d. Austri, and A. W. Strong, “Constraints on cosmic-ray propagation models from a global Bayesian analysis,” Astrophys. J.729(2011) 106,arXiv:1011.0037 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  64. [64]

    Cosmic ray propagation and dark matter in light of the latest AMS-02 data

    H.-B. Jin, Y.-L. Wu, and Y.-F. Zhou, “Cosmic ray propagation and dark matter in light of the latest AMS-02 data,”JCAP09(2015) 049,arXiv:1410.0171 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  65. [65]

    Bayesian analysis of cosmic-ray propagation: evidence against homogeneous diffusion

    G. J´ ohannessonet al., “Bayesian analysis of cosmic-ray propagation: evidence against homogeneous diffusion,”Astrophys. J.824no. 1, (2016) 16,arXiv:1602.02243 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  66. [66]

    Solution of heliospheric propagation: unveiling the local interstellar spectra of cosmic ray species

    M. J. Boschiniet al., “Solution of heliospheric propagation: unveiling the local interstellar spectra of cosmic ray species,”Astrophys. J.840no. 2, (2017) 115,arXiv:1704.06337 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  67. [67]

    Deciphering the local Interstellar spectra of primary cosmic ray species with HelMod

    M. J. Boschiniet al., “Deciphering the local Interstellar spectra of primary cosmic ray species with HelMod,”Astrophys. J.858no. 1, (2018) 61,arXiv:1804.06956 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  68. [68]

    Inference of the Local Interstellar Spectra of Cosmic-Ray Nuclei Z≤ 28 with the GalProp–HelMod Framework,

    M. J. Boschiniet al., “Inference of the Local Interstellar Spectra of Cosmic-Ray Nuclei Z≤ 28 with the GalProp–HelMod Framework,”Astrophys. J. Suppl.250no. 2, (2020) 27, arXiv:2006.01337 [astro-ph.HE]

    work page arXiv 2020

  69. [69]

    Implications of current nuclear cross sections on secondary cosmic rays with the upcoming DRAGON2 code,

    P. De La Torre Luque, M. N. Mazziotta, F. Loparco, F. Gargano, and D. Serini, “Implications of current nuclear cross sections on secondary cosmic rays with the upcoming DRAGON2 code,”JCAP03(2021) 099,arXiv:2101.01547 [astro-ph.HE]

    work page arXiv 2021

  70. [70]

    Markov chain Monte Carlo analyses of the flux ratios of B, Be and Li with the DRAGON2 code,

    P. D. L. T. Luque, M. N. Mazziotta, F. Loparco, F. Gargano, and D. Serini, “Markov chain Monte Carlo analyses of the flux ratios of B, Be and Li with the DRAGON2 code,”JCAP 07(2021) 010,arXiv:2102.13238 [astro-ph.HE]

    work page arXiv 2021

  71. [71]

    Propagation of cosmic rays in the AMS-02 era

    Q. Yuan, S.-J. Lin, K. Fang, and X.-J. Bi, “Propagation of cosmic rays in the AMS-02 era,” Phys. Rev. D95no. 8, (2017) 083007,arXiv:1701.06149 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  72. [72]

    Implications of Lithium to Oxygen AMS-02 spectra on our understanding of cosmic-ray diffusion,

    M. Korsmeier and A. Cuoco, “Implications of Lithium to Oxygen AMS-02 spectra on our understanding of cosmic-ray diffusion,”Phys. Rev. D103no. 10, (2021) 103016, arXiv:2103.09824 [astro-ph.HE]

    work page arXiv 2021

  73. [73]

    Testing Cosmic-Ray Propagation Scenarios with AMS-02 and Voyager Data,

    E. Silver and E. Orlando, “Testing Cosmic-Ray Propagation Scenarios with AMS-02 and Voyager Data,”Astrophys. J.963no. 2, (2024) 111,arXiv:2401.06242 [astro-ph.HE]. [76]AMSCollaboration, M. Aguilaret al., “Properties of Cosmic-Ray Sulfur and Determination of the Composition of Primary Cosmic-Ray Carbon, Neon, Magnesium, and Sulfur: Ten-Year Results from th...

    work page arXiv 2024

  74. [74]

    Galactic Cosmic Rays in the Local Interstellar Medium: Voyager 1 Observations and Model Results,

    A. C. Cummings, E. C. Stone, B. C. Heikkila, N. Lal, W. R. Webber, G. J´ ohannesson, I. V. Moskalenko, E. Orlando, and T. A. Porter, “Galactic Cosmic Rays in the Local Interstellar Medium: Voyager 1 Observations and Model Results,”Astrophys. J.831no. 1, (2016) 18. 37

    work page 2016

  75. [75]

    Systematic Investigation of Solar Modulation of Galactic Protons for Solar Cycle 23 using a Monte Carlo Approach with Particle Drift Effects and Latitudinal Dependence

    P. Bobiket al., “Systematic Investigation of Solar Modulation of Galactic Protons for Solar Cycle 23 using a Monte Carlo Approach with Particle Drift Effects and Latitudinal Dependence,”Astrophys. J.745(2012) 132,arXiv:1110.4315 [astro-ph.SR]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  76. [76]

    On the forward-backward-in-time approach for monte carlo solution of parker’s transport equation: One-dimensional case,

    P. Bobik, M. Boschini, S. Della Torre, M. Gervasi, D. Grandi, G. La Vacca, S. Pensotti, M. Putis, P. Rancoita, D. Rozza,et al., “On the forward-backward-in-time approach for monte carlo solution of parker’s transport equation: One-dimensional case,”Journal of Geophysical Research: Space Physics121no. 5, (2016) 3920–3930

    work page 2016

  77. [77]

    Propagation of Cosmic Rays in Heliosphere: the HelMod Model

    M. J. Boschini, S. Della Torre, M. Gervasi, G. La Vacca, and P. G. Rancoita, “Propagation of cosmic rays in heliosphere: The HELMOD model,”Adv. Space Res.62(2018) 2859–2879,arXiv:1704.03733 [astro-ph.SR]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  78. [78]

    HelMod in the works: from direct observations to the local interstellar spectrum of cosmic-ray electrons

    M. J. Boschiniet al., “HelMod in the works: from direct observations to the local interstellar spectrum of cosmic-ray electrons,”Astrophys. J.854no. 2, (2018) 94, arXiv:1801.04059 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  79. [79]

    The HelMod Model in the Works for Inner and Outer Heliosphere: from AMS to Voyager Probes Observations

    M. J. Boschini, S. Della Torre, M. Gervasi, G. La Vacca, and P. G. Rancoita, “The HelMod Model in the Works for Inner and Outer Heliosphere: from AMS to Voyager Probes Observations,”Adv. Space Res.64no. 12, (2019) 2459–2476,arXiv:1903.07501 [physics.space-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  80. [80]

    Forecasting of cosmic rays intensities with HelMod Model,

    M. J. Boschini, S. Della Torre, M. Gervasi, G. La Vacca, and P. G. Rancoita, “Forecasting of cosmic rays intensities with HelMod Model,”Adv. Space Res.70no. 9, (2022) 2649–2657

    work page 2022

Showing first 80 references.