Reheating of the Universe and evolution of the inflaton

The problem of the reheating of the Universe after inflation is considered. Our approach is based on the use, as "first principles," of the renormalized version of (a) the evolution equation for the mean value of an interacting scalar field and (b) the semiclassical Einstein equations. We...

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Publicado: 1989
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_05562821_v40_n4_p955_Mazzitelli
http://hdl.handle.net/20.500.12110/paper_05562821_v40_n4_p955_Mazzitelli
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Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_05562821_v40_n4_p955_Mazzitelli
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spelling paper:paper_05562821_v40_n4_p955_Mazzitelli2023-06-08T15:42:07Z Reheating of the Universe and evolution of the inflaton The problem of the reheating of the Universe after inflation is considered. Our approach is based on the use, as "first principles," of the renormalized version of (a) the evolution equation for the mean value of an interacting scalar field and (b) the semiclassical Einstein equations. We compute (for two different toy models) the characteristic time for the damping of the mean-value oscillations. We show that when the oscillations are damped the Universe becomes radiation dominated and inflation ends. The techniques used in this paper are those of quantum field theory in curved space-time and can be generalized to more realistic models. © 1989 The American Physical Society. 1989 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_05562821_v40_n4_p955_Mazzitelli http://hdl.handle.net/20.500.12110/paper_05562821_v40_n4_p955_Mazzitelli
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
description The problem of the reheating of the Universe after inflation is considered. Our approach is based on the use, as "first principles," of the renormalized version of (a) the evolution equation for the mean value of an interacting scalar field and (b) the semiclassical Einstein equations. We compute (for two different toy models) the characteristic time for the damping of the mean-value oscillations. We show that when the oscillations are damped the Universe becomes radiation dominated and inflation ends. The techniques used in this paper are those of quantum field theory in curved space-time and can be generalized to more realistic models. © 1989 The American Physical Society.
title Reheating of the Universe and evolution of the inflaton
spellingShingle Reheating of the Universe and evolution of the inflaton
title_short Reheating of the Universe and evolution of the inflaton
title_full Reheating of the Universe and evolution of the inflaton
title_fullStr Reheating of the Universe and evolution of the inflaton
title_full_unstemmed Reheating of the Universe and evolution of the inflaton
title_sort reheating of the universe and evolution of the inflaton
publishDate 1989
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_05562821_v40_n4_p955_Mazzitelli
http://hdl.handle.net/20.500.12110/paper_05562821_v40_n4_p955_Mazzitelli
_version_ 1768545333271330816

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