Free energy and entropy in Rindler and de Sitter space-times

TL;DR

This paper analyzes the free energy and entropy of a massive scalar field in de Sitter space-time at various temperatures, revealing horizon and interior contributions, and unusual state dependencies, with implications for Rindler space.

Contribution

It provides explicit formulas for free energy in de Sitter space at specific temperatures, highlighting the distinct horizon and interior contributions and their temperature dependence.

Findings

Free energy has 'area' and 'volume' contributions linked to horizon and interior.

Bulk free energy behavior varies with temperature and mass, especially for $eta<2 extpi$ and $eta>2 extpi$.

UV contributions to free energy depend on the quantum state, which is unusual.

Abstract

We investigate the free energy and entropy of the Gaussian massive scalar field theory in the static de Sitter space-time for arbitrary temperature. For the inverse temperatures of the form $\beta=2 \pi 2^k, \ \ k\in \mathbf{Z}$, in curvature units, we find the explicit form of the free energy and its derivatives with respect to the temperature. There are two types of contributions to the free energy: one is of the "area type" and can be attributed to the horizon, while the other is of the "volume type" and is associated with the interior of the space-time. The latter contribution in the odd-dimensional case in the limit of the week field (large mass or small Hubble constant) significantly depends on the temperature. Namely, for $ \beta<2\pi$, the free energy behaves as $ F^{bulk}_{\beta} \sim e^{- \beta \, m} $, while for $\beta>2\pi$ it behaves as $ F^{bulk}_{\beta} \sim e^{- 2 \, \pi \, m}$. We also show that even the leading UV contributions to the free energy significantly depend on the state of the theory, which is very unusual. We explain the origin and physical meaning of these observations. As the model example we consider the situation in the Rindler wedge of the flat space-time.