Radiative corrections from spectator fields cause the inflaton to evolve as an exponential of N_e squared during slow-roll inflation, unlike linear friction approximations, while producing spectator particles whose total number grows exponentially with e-folds.
Gravitational Waves from Isocurvature Perturbations of Spectator Scalar Fields
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A spectator scalar field with strong portal coupling to the inflaton sources a stochastic gravitational wave background reaching Ω_GW h² ∼ 10^{-11} at frequencies 10^7-10^8 Hz for benchmark parameters σ/λ ≃ 10^4 and T_reh = 2×10^{14} GeV.
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What spectators do during inflation
Radiative corrections from spectator fields cause the inflaton to evolve as an exponential of N_e squared during slow-roll inflation, unlike linear friction approximations, while producing spectator particles whose total number grows exponentially with e-folds.
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Gravitational Waves from Matter Perturbations of Spectator Scalar Fields
A spectator scalar field with strong portal coupling to the inflaton sources a stochastic gravitational wave background reaching Ω_GW h² ∼ 10^{-11} at frequencies 10^7-10^8 Hz for benchmark parameters σ/λ ≃ 10^4 and T_reh = 2×10^{14} GeV.