Heating up the cold bounce

Details Heating up the cold bounce Heating up the cold bounce

2004-06-11

arxiv.org/abs/hep-th/0406098v1

Class.Quant.Grav. 21 (2004) 4209-4230

Physics

High Energy Physics

High Energy Physics - Theory

28 pages, 13 figures

Scientific paper

10.1088/0264-9381/21/17/010

Self-dual string cosmological models provide an effective example of bouncing solutions where a phase of accelerated contraction smoothly evolves into an epoch of decelerated Friedmann--Robertson--Walker expansion dominated by the dilaton. While the transition to the expanding regime occurs at sub-Planckian curvature scales, the Universe emerging after the bounce is cold, with sharply growing gauge coupling. However, since massless gauge bosons (as well as other massless fields) are super-adiabatically amplified, the energy density of the maximally amplified modes re-entering the horizon after the bounce can efficiently heat the Universe. As a consequence the gauge coupling reaches a constant value, which can still be perturbative.

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