1998/12/31 by Jorma Louko, Kristin Schleich
Physics and Astronomy · #Black Holes and Theoretical Physics #Cosmology and Gravitation Theories #Quantum Electrodynamics and Casimir Effect #gr-qc #hep-th
paper · pdf · doi:10.1088/0264-9381/16/6/328
published as Class.Quant.Grav. 16 (1999) 2005-2021 · 22 pages, REVTex v3.1 with amsfonts and epsf, includes 2 eps figures. (v2: Minor typos corrected, references updated.)
openalex publication_date 1999/01/01 · arxiv created 1999/05/26 · arxiv updated 2009/11/30 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/04
We consider scalar field theory on the 3 de Sitter spacetime ( 3 dS), which is locally isometric to de Sitter space (dS) but has spatial topology 3 . We compare the Euclidean vacua on 3 dS and dS in terms of three quantities that are relevant for an inertial observer: (a) the stress-energy tensor; (b) the response of an inertial monopole particle detector; (c) the expansion of the Euclidean vacuum in terms of many-particle states associated with static coordinates centred at an inertial worldline. In all these quantities, the differences between 3 dS and dS turn out to fall off exponentially at early and late proper times along the inertial trajectory. In particular, (b) and (c) yield at early and late proper times in 3 dS the usual thermal result for the de Sitter Hawking temperature. This conforms to what one might call an exponential law: in expanding locally de Sitter spacetimes, differences due to global topology should fall off exponentially in the proper time.