Scalar Casimir densities induced by a cylindrical shell in de Sitter spacetime

TL;DR

This paper calculates the quantum vacuum effects of a scalar field around a cylindrical shell in de Sitter spacetime, revealing how boundary conditions and the spacetime curvature influence energy densities and fluxes.

Contribution

It provides a detailed analysis of the vacuum expectation values and energy-momentum tensor for a scalar field with Robin boundary conditions in de Sitter space, including new insights into boundary-induced effects.

Findings

Shell-induced vacuum energy-momentum tensor has off-diagonal energy flux.

Vacuum energy density and flux can be positive or negative depending on parameters.

Decay of vacuum expectation values with distance follows a power-law, faster for Neumann conditions.

Abstract

We evaluate the positive-frequency Wightman function, the vacuum expectation values (VEVs) of the field squared and the energy-momentum tensor for a massive scalar field with general curvature coupling for a cylindrical shell in background of dS spacetime. The field is prepared in the Bunch-Davies vacuum state and on the shell the corresponding operator obeys Robin boundary condition. In the region inside the shell and for non-Neumann boundary conditions, the Bunch-Davies vacuum is a physically realizable state for all values of the mass and curvature coupling parameter. For both interior and exterior regions, the VEVs are decomposed into boundary-free dS and shell-induced parts. We show that the shell-induced part of the vacuum energy-momentum tensor has a nonzero off-diagonal component corresponding to the energy flux along the radial direction. Unlike to the case of a shell in Minkowski bulk, for dS background the axial stresses are not equal to the energy density. In dependence of the mass and of the coefficient in the boundary condition, the vacuum energy density and the energy flux can be either positive or negative. The influence of the background gravitational field on the boundary-induced effects is crucial at distances from the shell larger than the dS curvature scale. In particular, the decay of the VEVs with the distance is power-law (monotonic or oscillatory with dependence of the mass) for both massless and massive fields. For Neumann boundary condition the decay is faster than that for non-Neumann conditions.