The first search for scalar-induced gravitational waves via pulsar parameter drifts yields f_PBH < 10^{-10} (95% CL) for PBH masses 0.3 to 4e4 solar masses, strongly disfavoring a primordial black hole origin for LVK binary black holes.
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Constraints on primordial black holes
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Primordial black hole formation from slow first-order phase transitions remains viable if slow reheating after supercooling creates an early matter-dominated era allowing small overdensities to grow, producing black holes with large spins.
Full numerical N-body treatment is required for reliable gravitational wave predictions from nonspherical collapse in early matter-dominated eras, with resulting spectra mappable to detector sensitivities via horizon mass and reheating temperature.
A quenched-disorder approach with Schwinger-Keldysh path integrals produces an averaged density matrix for gravitational waves that separates phase-suppressing exponential terms from oscillatory corrections to coherent propagation.
In the ADD extra-dimension model, microscopic primordial black holes undergo runaway accretion and grow to macroscopic scales, allowing them to comprise all dark matter with initial abundances as low as 10^{-44}.
Asteroid-mass primordial black holes induce a Riemann tidal splitting of the 2P_{3/2} hydrogen state, turning the 9.9 GHz line into a ~2 GHz bandwidth gravitational spectral radio forest in H II regions with accretion-enhanced emission measure.
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.
Derives stochastic equations from Schwinger-Keldysh formalism that include quantum diffusion and classical metric perturbations for non-perturbative ultra-slow-roll inflation, validated on Starobinsky and critical Higgs models.
High-energy neutrino telescopes constrain sub-asteroid mass primordial black holes with extended mass functions as dark matter, yielding limits slightly weaker than but independent of gamma-ray bounds.
Monte Carlo solutions to the Smoluchowski coagulation equation yield runaway timescales and mass evolution for primordial black hole clusters at different redshifts based on cluster properties.
PBHs generated by axion inflation with gauge-field coupling can comprise all dark matter in the asteroidal mass range while producing a LISA-measurable stochastic GW background.
Repulsive-like primordial black holes in the Swiss-cheese framework produce quasi-de Sitter expansion, enabling inflation with evaporation reheating and acting as early dark energy for certain masses and densities.
Purely quadratic non-Gaussianity from tachyonic instability allows narrow curvature spectra to exponentially suppress primordial black hole overproduction via correlation coefficient ρ approaching -1 while retaining sizable scalar-induced gravitational waves.
Upper bounds on the dark matter fraction in MACHOs of 10^3 to 10^7 solar masses are derived from limits on distortions to the global 21-cm signal at z~17, z~89, and z>300.
Memory-burden backreaction deforms the Hawking spectrum to suppress its high-energy tail, lowering total luminosity and neutrino flux by a factor set by a single suppression parameter and thereby relaxing IceCube bounds on primordial black hole dark matter.
CMB data limits the s-wave annihilation cross section of thermal dark matter particles to ≲ 10^{-30} cm³/s scaled by PBH fraction and mass for PBHs heavier than ~10^{-10} solar masses.
LOFAR2.0, FAST Core Array and BINGO can constrain the PBH dark matter fraction f_PBH below 0.16-0.39 for masses above 10^{-2} to 10 solar masses via FRB lensing statistics.
Baselines of 8-11 ms light travel time for two CE detectors provide a reasonable compromise for BBH sky localization, with third detectors eliminating multimodality for most or all events.
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