Thermal Interpretation of Infrared Dynamics in de Sitter

TL;DR

This paper demonstrates that the infrared dynamics of a scalar field in de Sitter space can be understood as a thermal Brownian motion at the de Sitter temperature, leading to a thermal equilibrium state and enabling non-perturbative stress tensor calculations.

Contribution

It derives an effective stochastic action for scalar field fluctuations in de Sitter space, generalizing Starobinsky's stochastic inflation framework and linking infrared dynamics to thermalization.

Findings

Infrared scalar field dynamics resemble Brownian motion at de Sitter temperature.

The equilibrium state is a de Sitter invariant thermal Gibbs distribution.

Allows non-perturbative computation of the stress-energy tensor in de Sitter space.

Abstract

The infrared dynamics of a light, minimally coupled scalar field in de Sitter spacetime with Ricci curvature $R=12H$, averaged over horizon sized regions of physical volume $V_H=\frac{4\pi}{3}\left(\frac{1}{H}\right)^3$, can be interpreted as Brownian motion in a medium with de Sitter temperature $T_{DS}=\frac{\hbar H}{2\pi}$. We demonstrate this by directly deriving the effective action of scalar field fluctuations with wavelengths larger than the de Sitter curvature radius and generalizing Starobinsky's seminal results on stochastic inflation. The effective action describes stochastic dynamics and the fluctuating force drives the field to an equilibrium characterized by a thermal Gibbs distribution at temperature $T_{DS}$ which corresponds to a de Sitter invariant state. Hence, approach towards this state can be interpreted as thermalization. We show that the stochastic kinetic energy of the coarse-grained description corresponds to the norm of $\partial_\mu\phi$ and takes a well defined value per horizon volume $\frac{1}{2}\langle \left(\nabla\phi\right)^2\rangle = - \frac{1}{2}T_{DS}/V_H$. This approach allows for the non-perturbative computation of the de Sitter invariant stress energy tensor $\langle T_{\mu\nu} \rangle$ for an arbitrary scalar potential.