Gravitational waves from a universe filled with primordial black holes
Résumé
Ultra-light primordial black holes, with masses m PBH < 109g, evaporate before big-bang nucleosynthesis and can therefore not be directly constrained. They can however be so abundant that they dominate the universe content for a transient period (before reheating the universe via Hawking evaporation). If this happens, they support large cosmological fluctuations at small scales, which in turn induce the production of gravitational waves through second-order effects. Contrary to the primordial black holes, those gravitational waves survive after evaporation, and can therefore be used to constrain such scenarios. In this work, we show that for induced gravitational waves not to lead to a backreaction problem, the relative abundance of black holes at formation, denoted ΩPBH,f, should be such that ΩPBH,f < 10-4(m PBH/109g)-1/4. In particular, scenarios where primordial black holes dominate right upon their formation time are all excluded (given that m PBH > 10 g for inflation to proceed at ρ1/4 < 1016 GeV). This sets the first constraints on ultra-light primordial black holes.
Mots clés
physics of the early universe
gravitational waves / theory
primordial black holes
black hole: primordial
black hole: mass
gravitational radiation: induced
nucleosynthesis: big bang
formation: time
black hole: formation
black hole: evaporation
back reaction
space-time: fluctuation
reheating
inflation
evaporation
gravitational radiation: emission
power spectrum: tensor
power spectrum
matter: power spectrum
perturbation: scalar
tensor: energy-momentum
energy: density
gauge