Extends the stochastic inflation formalism to a wide class of scalar-tensor theories by mapping EFT of dark energy coefficients to stochastic equations of motion.
Tomberg, (2024)
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The conventional truncation in stochastic inflation is inconsistent because quadratic-noise contributions are the same perturbative order as the deterministic non-Markovian corrections.
Spectral solution of the Fokker-Planck operator for hilltop constant-roll inflation shows rare crossing trajectories dominate the mean, so the median yields a coarse-grained ΔN distribution whose exponential tail flattens into a peak near maximal value.
Numerical simulations using BSSN numerical relativity reproduce the expected evolution of stochastic inflation in both slow-roll and ultra slow-roll regimes while retaining gradients and anisotropic expansion.
citing papers explorer
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Stochastic scalar-tensor inflation and beyond
Extends the stochastic inflation formalism to a wide class of scalar-tensor theories by mapping EFT of dark energy coefficients to stochastic equations of motion.
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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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Stochastic constant-roll inflation beyond the hilltop with the spectral method
Spectral solution of the Fokker-Planck operator for hilltop constant-roll inflation shows rare crossing trajectories dominate the mean, so the median yields a coarse-grained ΔN distribution whose exponential tail flattens into a peak near maximal value.
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Stochastic Inflation in Numerical Relativity
Numerical simulations using BSSN numerical relativity reproduce the expected evolution of stochastic inflation in both slow-roll and ultra slow-roll regimes while retaining gradients and anisotropic expansion.