Finite temperature scalar field theory in the early universe.

Details Finite temperature scalar field theory in the early universe. Finite temperature scalar field theory in the early universe.

Jan 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991anphy.205....1l&link_type=abstract

Ann. Phys. (N.Y.), Vol. 205, No. 1, p. 1 - 28

Physics

17

Early Universe, Cosmology: Inflationary Universe, Cosmology: Robertson-Walker Metric

Scientific paper

The authors study a scalar Higgs field in an expanding Robertson-Walker geometry, using the real time formulation of Semenoff and Weiss. It is shown that the density matrix associated with the Hamiltonian at a sharp time describes a state for which perturbation theory is not renormalizable and an alternative, renormalizable characterization of thermal equilibrium is given. They calculate the thermal quantum fluctuations surrounding a classical field and discuss the characteristic time scales occurring in the evolution of a scalar field from an initial radiation dominated phase of thermal equilibrium to an unstable, inflationary de Sitter phase.

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