Non-vacuum initial states for the cosmological perturbations and the back-reaction problem of inflation

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dc.creatorGangui, Alejandro
dc.creatorMartin, Jerome
dc.creatorSakellariadou, Mairi
dc.date2002-06-03
dc.date.accessioned2026-07-07T02:03:51Z
dc.date.available2026-07-07T02:03:51Z
dc.descriptionIn the framework of Inflationary theory, the assumption that the quantum state of the perturbations is a non-vacuum state leads to a difficulty: non-vacuum initial states imply, in general, a large energy density of inflaton field quanta, not of a cosmological term type, that could prevent the inflationary phase. In this short note, we discuss in detail why this is so, keeping an eye on possible non-Gaussian features due to considering generic non-vacuum initial states.
dc.descriptionTo appear in the Proceedings of the XXXVIIth Rencontres de Moriond on ``The Cosmological Model'', Les Arcs, France, March 16-23, 2002
dc.identifierhttps://arxiv.org/abs/astro-ph/0206023
dc.identifierhttp://arxiv.org/abs/astro-ph/0206023
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/4535
dc.subjectAstrophysics
dc.subjectGeneral Relativity and Quantum Cosmology
dc.subjectHigh Energy Physics - Phenomenology
dc.subjectHigh Energy Physics - Theory
dc.titleNon-vacuum initial states for the cosmological perturbations and the back-reaction problem of inflation
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