Propagators for a Scalar Field in a Homogeneous Expanding Universe. I ---Case of the Friedmann Universes---

Details Propagators for a Scalar Field in a Homogeneous Expanding Universe. I ---Case of the Friedmann Universes--- Propagators for a Scalar Field in a Homogeneous Expanding Universe. I ---Case of the Friedmann Universes---

Apr 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976pthph..55.1116n&link_type=abstract

Progress of Theoretical Physics, Vol. 55, No. 4, pp. 1116-1132

Physics

4

Scientific paper

In view of a recent interest in the quantum field-theoretical creation of particles in a big-bang universe (which, via the problem how their vacuum state should be defined, will be connected with their propagators whose structure depends also on that of the universe), our previous formulae for bi-scalar Green's functions corresponding to a massless scalar field in the radiation- and matter-dominated stages of the Friedmann universe with flat 3-space are extended in a classical level. One is to derive the formulae for a massive scalar field in the same universe, and another lies in deriving the ones applicable to the respective stages of a closed universe with spherical topology. As an application, we discuss a massless scalar field (e.g., photons or gravitons defined suitably) and its physical property in the cases where its source distribution is spatially uniform and where that is of a delta-singularity. It is shown that the energy-momentum tensor in the first case is formally the same as that for a perfect fluid whose sound velocity relative to the light velocity is unity, while the tensor in the second case leads naturally to Robertson's formula for the apparent luminosity of a receding galaxy. The behavior of photons or gravitons generated from a turbulent medium in an early universe is also dealt with.

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