The stochastic noise amplitude is modified to (H/2π) * sqrt(1 + ΔP_R / P0_R) to account for one-loop corrections in interacting theories, demonstrated in a three-phase SR-USR-SR setup for PBH formation.
2023b, arXiv e-prints
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Derives all-order Hamiltonians via EFT of inflation for USR models and shows L-loop corrections to CMB-scale perturbations scale as (ΔN P_e L)^L, exiting perturbative control at L=4 for typical ΔN≈2.5.
In USR inflation with an idealized instantaneous sharp transition to slow-roll, higher loop corrections to curvature perturbations on CMB scales grow rapidly with loop order L and may exit perturbative control.
A PBH fraction of about 0.1 as dark matter, with 1% in stellar-mass range, produces the observed SGWB amplitude via dynamical friction and hierarchical mergers while explaining JWST early SMBHs.
citing papers explorer
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Stochastic Inflation with Interacting Noises
The stochastic noise amplitude is modified to (H/2π) * sqrt(1 + ΔP_R / P0_R) to account for one-loop corrections in interacting theories, demonstrated in a three-phase SR-USR-SR setup for PBH formation.
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Hamiltonians to all Orders in Perturbation Theory and Higher Loop Corrections in Single Field Inflation with PBHs Formation
Derives all-order Hamiltonians via EFT of inflation for USR models and shows L-loop corrections to CMB-scale perturbations scale as (ΔN P_e L)^L, exiting perturbative control at L=4 for typical ΔN≈2.5.
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Non-Perturbative Hamiltonian and Higher Loop Corrections in USR Inflation
In USR inflation with an idealized instantaneous sharp transition to slow-roll, higher loop corrections to curvature perturbations on CMB scales grow rapidly with loop order L and may exit perturbative control.
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Primordial Black Hole contribution to the stochastic background of Gravitational Waves
A PBH fraction of about 0.1 as dark matter, with 1% in stellar-mass range, produces the observed SGWB amplitude via dynamical friction and hierarchical mergers while explaining JWST early SMBHs.