Self-consistent spherical accretion simulations show cooling-enhanced growth of PBHs with radiative efficiency ~10^{-2} in the bremsstrahlung regime, yielding a critical seed mass of ~10^{-16} M_sun to consume a solar-mass star in a Hubble time.
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New cosmological constraints on primordial black holes
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abstract
We update the constraints on the fraction of the Universe going into primordial black holes in the mass range 10^9--10^17 g associated with the effects of their evaporations on big bang nucleosynthesis and the extragalactic photon background. We include for the first time all the effects of quark and gluon emission by black holes on these constraints and account for the latest observational developments. We then discuss the other constraints in this mass range and show that these are weaker than the nucleosynthesis and photon background limits, apart from a small range 10^13--10^14 g, where the damping of cosmic microwave background anisotropies dominates. Finally we review the gravitational and astrophysical effects of nonevaporating primordial black holes, updating constraints over the broader mass range 1--10^50 g.
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representative citing papers
Non-singular gravity with regulator ℓ induces a PBH mass gap ~c²ℓ/G and a stronger Carr criterion δ_H > 2GM_gap/R_H - 1 when R_H ~ ℓ.
Accounting for the minimal mass spread of primordial black holes from gravitational collapse suppresses the Poltergeist GW background to the level of generic scalar-induced signals and reopens ultra-light PBH parameter space.
Stupendously large black holes cast shadows on the CMB that rule out masses above 10^17 solar masses within the last scattering surface and limit their density parameter to below 10^-5 for masses 10^15 to 10^18 solar masses.
Bumblebee gravity enhances primordial black hole abundance through three mechanisms, but the model harbors a ghost instability and a tachyonic instability that make it cosmologically unviable.
Scaling monopoles generate PBHs via stochastic overdensities and GWs with correlated spectra, potentially with magnetically charged PBHs as a signature if the scaling ends via gauge boson mass.
Incorporating the general-relativity mass tail df_PBH/d ln M ∝ M^3.78 smooths PBH evaporation, suppresses the scalar-induced GW signal by orders of magnitude, and reopens the ultra-light PBH window for the hot Big Bang.
Primordial black holes generate up to 30% amplitude VAO wiggles in 21 cm signals from the Dark Ages at redshifts 20-40 even at dark matter fractions as low as 10^-13.
Hotspots around light primordial black holes cool faster in an expanding universe following T_plt ∝ t^{-11/15} and vanish completely in finite time, unlike everlasting hotspots in flat spacetime.
EHT dimensionless shadow diameters plus stellar-dynamical mass priors constrain Einasto central density to ρ₀ ≲ 10^{-11} M⊙/pc³ (1σ) for Sgr A*, with weaker bounds for M87*.
Photon-to-graviton conversion in blazar jets dominates a new graviton background that sets a floor for high-frequency GW detectors, analogous to the neutrino floor.
PBH production from slow phase transitions with delayed reheating is modeled via peak theory and Monte Carlo simulations, showing extreme sensitivity to reheating efficiency and potential to explain all dark matter.
A model in which inflaton energy goes exclusively to a dark sector, delaying SM thermalization until a false-vacuum decay produces a GW background with present-day Omega_GW up to 3e-8.
PBH masses near 10^3 kg allow Hawking evaporation to reheat the universe while Planckian remnants comprise all present-day DM without fine-tuning initial abundance, yielding testable GW signals.
Calculations indicate AMEGO-X could detect PBH transits within 0.1 AU while HAWC and LHAASO could observe explosions out to 0.1-0.5 pc, with future events at ~1000 AU potentially producing measurable electromagnetic signals unlike the 2023 KM3NeT neutrino candidate.
In excursion set theory with colored noises, the low-mass tail of the PBH mass function differs from Carr's formula because correlated noises end the degeneracy of formation probabilities, though Carr's formula remains practical near the characteristic mass for smooth Fourier-space window functions.
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.
Tensor perturbations from FOPT and domain-wall sources are claimed to induce second-order scalar perturbations large enough to form primordial black holes, potentially all of the dark matter.
Inflationary magnetic fields induce curvature perturbations that form ultralight PBHs, generating a stochastic GW background with model-specific features.
Deformed alpha-attractor T-models with a Gaussian feature near the minimum yield more smaller shorter-lived oscillons during self-resonance preheating, suppressing energy in oscillons and altering the high-frequency gravitational wave tail while leaving low frequencies unchanged.
Hawking-evaporating primordial black holes could boost light dark matter to detectable energies, and the new electron-recoil constraints from XENONnT, LZ, and PandaX-4T tighten limits on its mass and cross-section.
Galactic synchrotron emissions above 20 MHz can set tighter upper limits on the abundance of primordial black holes with masses above 10^16 grams than previous cosmic-ray electron data.
Thermal bath corrections derived via thermofield dynamics enhance the evaporation rate of primordial black holes, shortening their lifetimes relative to zero-temperature calculations.
Regular primordial black holes can evaporate completely like singular ones and yield the observed dark matter density under modified cosmological constraints.
citing papers explorer
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Gravitational Waves from Black Hole Reheating: The Scalar-Induced Component
Accounting for the minimal mass spread of primordial black holes from gravitational collapse suppresses the Poltergeist GW background to the level of generic scalar-induced signals and reopens ultra-light PBH parameter space.
- Primordial Black Holes: A Review of Formation and Evolution