1D Supergravity FLRW Model of Starobinsky

We study two homogeneous supersymmetric extensions for the <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>)</mo></mrow&...

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Autores principales:	Nephtalí E. Martínez-Pérez, Cupatitzio Ramírez-Romero, Víctor M. Vázquez-Báez
Formato:	article
Lenguaje:	EN
Publicado:	MDPI AG 2021
Materias:	local supersymmetry model of starobinsky cosmic inflation Elementary particle physics QC793-793.5
Acceso en línea:	https://doaj.org/article/9b42092433574a2a8b372819c2032e1a
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spelling	oai:doaj.org-article:9b42092433574a2a8b372819c2032e1a2021-11-25T19:09:54Z1D Supergravity FLRW Model of Starobinsky10.3390/universe71104492218-1997https://doaj.org/article/9b42092433574a2a8b372819c2032e1a2021-11-01T00:00:00Zhttps://www.mdpi.com/2218-1997/7/11/449https://doaj.org/toc/2218-1997We study two homogeneous supersymmetric extensions for the <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>)</mo></mrow></semantics></math></inline-formula> modified gravity model of Starobinsky with the FLRW metric. The actions are defined in terms of a superfield <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mi mathvariant="script">R</mi></semantics></math></inline-formula> that contains the FLRW scalar curvature. One model has N = 1 local supersymmetry, and its bosonic sector is the Starobinsky action; the other action has N = 2, its bosonic sector contains, in additional to Starobinsky, a massive scalar field without self-interaction. As expected, the bosonic sectors of these models are consistent with cosmic inflation, as we show by solving numerically the classical dynamics. Inflation is driven by the <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mi>R</mi><mn>2</mn></msup></semantics></math></inline-formula> term during the large curvature regime. In the N = 2 case, the additional scalar field remains in a low energy state during inflation. Further, by means of an additional superfield, we write equivalent tensor-scalar-like actions from which we can give the Hamiltonian formulation.Nephtalí E. Martínez-PérezCupatitzio Ramírez-RomeroVíctor M. Vázquez-BáezMDPI AGarticlelocal supersymmetrymodel of starobinskycosmic inflationElementary particle physicsQC793-793.5ENUniverse, Vol 7, Iss 449, p 449 (2021)
institution	DOAJ
collection	DOAJ
language	EN
topic	local supersymmetry model of starobinsky cosmic inflation Elementary particle physics QC793-793.5
spellingShingle	local supersymmetry model of starobinsky cosmic inflation Elementary particle physics QC793-793.5 Nephtalí E. Martínez-Pérez Cupatitzio Ramírez-Romero Víctor M. Vázquez-Báez 1D Supergravity FLRW Model of Starobinsky
description	We study two homogeneous supersymmetric extensions for the <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>)</mo></mrow></semantics></math></inline-formula> modified gravity model of Starobinsky with the FLRW metric. The actions are defined in terms of a superfield <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mi mathvariant="script">R</mi></semantics></math></inline-formula> that contains the FLRW scalar curvature. One model has N = 1 local supersymmetry, and its bosonic sector is the Starobinsky action; the other action has N = 2, its bosonic sector contains, in additional to Starobinsky, a massive scalar field without self-interaction. As expected, the bosonic sectors of these models are consistent with cosmic inflation, as we show by solving numerically the classical dynamics. Inflation is driven by the <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mi>R</mi><mn>2</mn></msup></semantics></math></inline-formula> term during the large curvature regime. In the N = 2 case, the additional scalar field remains in a low energy state during inflation. Further, by means of an additional superfield, we write equivalent tensor-scalar-like actions from which we can give the Hamiltonian formulation.
format	article
author	Nephtalí E. Martínez-Pérez Cupatitzio Ramírez-Romero Víctor M. Vázquez-Báez
author_facet	Nephtalí E. Martínez-Pérez Cupatitzio Ramírez-Romero Víctor M. Vázquez-Báez
author_sort	Nephtalí E. Martínez-Pérez
title	1D Supergravity FLRW Model of Starobinsky
title_short	1D Supergravity FLRW Model of Starobinsky
title_full	1D Supergravity FLRW Model of Starobinsky
title_fullStr	1D Supergravity FLRW Model of Starobinsky
title_full_unstemmed	1D Supergravity FLRW Model of Starobinsky
title_sort	1d supergravity flrw model of starobinsky
publisher	MDPI AG
publishDate	2021
url	https://doaj.org/article/9b42092433574a2a8b372819c2032e1a
work_keys_str_mv	AT nephtaliemartinezperez 1dsupergravityflrwmodelofstarobinsky AT cupatitzioramirezromero 1dsupergravityflrwmodelofstarobinsky AT victormvazquezbaez 1dsupergravityflrwmodelofstarobinsky
_version_	1718410233088311296

1D Supergravity FLRW Model of Starobinsky

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