Simple Equations for Cosmological Matter and Inflaton Field Interactions

Eckhard Rebhan; Thorsten Battefeld

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arXiv · hep-th/0303019

Simple Equations for Cosmological Matter and Inflaton Field Interactions

Eckhard Rebhan·Thorsten Battefeld

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Abstract

A simple model for the reheating of the universe after inflation is studied in which an essentially inhomogeneous scalar field representing matter is coupled to an essentially homogeneous scalar inflaton field. Through this coupling, the potential determining the evolution of the inflaton field is made time-dependent. Due to this the frequency of parametric resonance becomes time dependent, making the reheating process especially effective. All fields including the gravitational field are initially simplified by expanding each in terms of the respective homogeneity or inhomogeneity. Employing only the lowest order of this expansion, we space-average, and introduce all independent averages as new variables. This leads to a hierarchy of equations for the spatial moments of the fields and their derivatives. A small expansion parameter permits a truncation to lowest order, yielding a closed system of 5 coupled nonlinear first order differential equations. For a parabolic potential, the energy densities of the matter and inflaton fields oscillate chaotically around each other from the end of inflation until they reach extremely small values. The average period of preponderance of one of the two continuously increases in this process. We discuss that this may provide one clue to a solution of the coincidence problem. For a Mexican hat potential we can easily obtain and understand dynamical symmetry breaking.

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Eckhard Rebhan, Thorsten Battefeld. 2003-03-03. Simple Equations for Cosmological Matter and Inflaton Field Interactions. https://arxiv.org/abs/hep-th/0303019

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