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

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 is an element of 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-beta(bulk) similar to e(-beta m), while for beta > 2 pi it behaves as F-beta(bulk) similar to 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.

Automated summary

We investigate the free energy and entropy of the Gaussian massive scalar field theory in static de Sitter space-time for arbitrary temperature. For the inverse temperatures of the form beta = 2 pi 2(k), k is an element of Z, in curvature units, we find the explicit form of the free energy and its derivatives with respect to 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 significantly depends on temperature in the odd-dimensional case for the limit of weak field (large mass or small Hubble constant).