Stochastic binary tree method computes compaction function in inflation to distinguish type I/II PBH fluctuations, finding broader mass distributions and type-II dominance in quantum regimes of a toy model.
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Exact solution of time-reversed stochastic inflation in the quantum well yields curvature perturbation distributions with faster-decaying exponential tails than forward stochastic inflation.
The conventional truncation in stochastic inflation is inconsistent because quadratic-noise contributions are the same perturbative order as the deterministic non-Markovian corrections.
Stochastic effects in multifield inflation make the number of fields relevant for e-fold statistics and power spectrum, with a general formula for higher moments and an upper bound on fields for successful inflation.
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.
citing papers explorer
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Compaction function in stochastic inflation: a \texttt{FOREST} of type I and II primordial black holes
Stochastic binary tree method computes compaction function in inflation to distinguish type I/II PBH fluctuations, finding broader mass distributions and type-II dominance in quantum regimes of a toy model.
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Time-reversed stochastic inflation in the quantum well
Exact solution of time-reversed stochastic inflation in the quantum well yields curvature perturbation distributions with faster-decaying exponential tails than forward stochastic inflation.
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A consistent formulation of stochastic inflation I: Non-Markovian effects and issues beyond linear perturbations
The conventional truncation in stochastic inflation is inconsistent because quadratic-noise contributions are the same perturbative order as the deterministic non-Markovian corrections.
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Multifield stochastic inflation: Relevance of number of fields in statistical moments
Stochastic effects in multifield inflation make the number of fields relevant for e-fold statistics and power spectrum, with a general formula for higher moments and an upper bound on fields for successful inflation.
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Nonperturbative stochastic inflation in perturbative dynamical background
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.