Kinetic vs. Thermal-Field-Theory Approach to Cosmological Perturbations

Details Kinetic vs. Thermal-Field-Theory Approach to Cosmological Perturbations Kinetic vs. Thermal-Field-Theory Approach to Cosmological Perturbations

1994-03-16

arxiv.org/abs/gr-qc/9403032v1

Phys.Rev. D50 (1994) 2541-2559

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

31 pages, 10 figures (uu encoded ps-file appended), REVTEX 3.0, DESY 94-040 / TUW-93-23

Scientific paper

10.1103/PhysRevD.50.2541

A closed set of equations for the evolution of linear perturbations of homogeneous, isotropic cosmological models can be obtained in various ways. The simplest approach is to assume a macroscopic equation of state, e.g.\ that of a perfect fluid. For a more refined description of the early universe, a microscopic treatment is required. The purpose of this paper is to compare the approach based on classical kinetic theory to the more recent thermal-field-theory approach. It is shown that in the high-temperature limit the latter describes cosmological perturbations supported by collisionless, massless matter, wherein it is equivalent to the kinetic theory approach. The dependence of the perturbations in a system of a collisionless gas and a perfect fluid on the initial data is discussed in some detail. All singular and regular solutions are found analytically.

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