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Title: On post-inflation validity of perturbation theory in Horndeski scalar-tensor models
Author: Germani, Cristiano
Kudryashova, Nina
Watanabe, Yuki
Keywords: Cosmologia quàntica
Relativitat general (Física)
Partícules (Física nuclear)
Quantum cosmology
General relativity (Physics)
Particles (Nuclear physics)
Issue Date: 8-Aug-2016
Publisher: Institute of Physics (IOP)
Abstract: By using the newtonian gauge, we re-confirm that, as in the minimal case, the re-scaled Mukhanov-Sasaki variable is conserved leading to a constraint equation for the Newtonian potential. However, conversely to the minimal case, in Horndeski theories, the super-horizon Newtonian potential can potentially grow to very large values after inflation exit. If that happens, inflationary predictability is lost during the oscillating period. When this does not happen, the perturbations generated during inflation can be standardly related to the CMB, if the theory chosen is minimal at low energies. As a concrete example, we analytically and numerically discuss the new Higgs inflationary case. There, the Inflaton is the Higgs boson that is non-minimally kinetically coupled to gravity. During the high-energy part of the post-inflationary oscillations, the system is anisotropic and the Newtonian potential is largely amplified. Thanks to the smallness of today's amplitude of curvature perturbations, however, the system stays in the linear regime, so that inflationary predictions are not lost. At low energies, when the system relaxes to the minimal case, the anisotropies disappear and the Newtonian potential converges to a constant value. We show that the constant value to which the Newtonian potential converges is related to the frozen part of curvature perturbations during inflation, precisely like in the minimal case.
Note: Versió postprint del document publicat a:
It is part of: Journal of Cosmology and Astroparticle Physics, 2016, vol. 2016
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ISSN: 1475-7516
Appears in Collections:Articles publicats en revistes (Institut de Ciències del Cosmos (ICCUB))

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