Stochastic Inflation with Interacting Noises

TL;DR

This paper extends the stochastic δN formalism to include interaction effects in noise amplitudes during inflation, incorporating quantum corrections to improve the modeling of primordial fluctuations.

Contribution

It introduces a modified stochastic δN formalism accounting for quantum loop corrections in noise amplitudes during inflation.

Findings

Derived the modified noise amplitude including one-loop corrections.

Applied the formalism to a three-phase inflationary setup for PBH formation.

Showed the noise amplitude is corrected by a factor involving the fractional power spectrum correction.

Abstract

Stochastic $\delta N$ formalism is a powerful tool to calculate the cosmological correlators non-perturbatively. However, it requires the initial data for the amplitude of the noise on the initial flat hypersurface which for a free theory during inflation is fixed to be $\frac{H}{2 \pi}$. In this work, we study the setups where the underlying theory involves interactions and the stochastic noises inherit these interactions. We extend the stochastic $\delta N$ formalism to these setups and rewrite the corresponding Langevin and Fokker-Planck equations in which the QFT corrections in the amplitude of the noises are taken into account. As an example, in the three-phase SR-USR-SR setup which is employed for PBHs formation, the modification in the amplitude of noise is calculated from the one-loop corrections in power spectrum via in-in formalism. We show that in these setups the amplitude of the stochastic noise is modified to $\frac{H}{2 \pi} \Big(1+ \frac{ \Delta {\cal P}_{\cal R} }{ {\cal P}^{(0)}_{ {\cal R} } }\Big)^{\frac{1}{2}}$ in which $ \frac{\Delta {\cal P}_{\cal R} }{ {\cal P}^{(0)}_{{\cal R} } }$ is the fractional one-loop correction in power spectrum.