Cosmological Model with Interconnection between Dark Energy and Matter

It is accepted in the present cosmology model that the scalar field, which is responsible for the inflation stage in the early universe, transforms completely into matter, and the accelerated universe expansion is presently governed by dark energy (DE), whose origin is not connected with the inflati...

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Autor principal:	Gennady S. Bisnovatyi-Kogan
Formato:	article
Lenguaje:	EN
Publicado:	MDPI AG 2021
Materias:	dark energy dark matter Hubble constant Elementary particle physics QC793-793.5
Acceso en línea:	https://doaj.org/article/c94604087dfb4634838ff0355898e704
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spelling	oai:doaj.org-article:c94604087dfb4634838ff0355898e7042021-11-25T19:09:34ZCosmological Model with Interconnection between Dark Energy and Matter10.3390/universe71104122218-1997https://doaj.org/article/c94604087dfb4634838ff0355898e7042021-10-01T00:00:00Zhttps://www.mdpi.com/2218-1997/7/11/412https://doaj.org/toc/2218-1997It is accepted in the present cosmology model that the scalar field, which is responsible for the inflation stage in the early universe, transforms completely into matter, and the accelerated universe expansion is presently governed by dark energy (DE), whose origin is not connected with the inflationary scalar field. We suppose here that dark matter (DM) has a common origin with a small variable component of dark energy (DEV). We suggest that DE may presently have two components, one of which is the Einstein constant <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mi mathvariant="normal">Λ</mi></semantics></math></inline-formula>, and another, smaller component DEV (<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi mathvariant="normal">Λ</mi><mi>V</mi></msub></semantics></math></inline-formula>) comes from the remnants of the scalar field responsible for inflation, which gave birth to the origin of presently existing matter. In this note we consider only the stages of the universe expansion after recombination, <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>z</mi><mo>≃</mo><mn>1100</mn></mrow></semantics></math></inline-formula>, when DM was the most abundant component of the matter, therefore we suggest for simplicity that a connection exists between DM and DEV so that the ratio of their densities remains constant over all the stages after recombination, <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><msub><mi>ρ</mi><mrow><mi>D</mi><mi>M</mi></mrow></msub><mo>=</mo><mi>α</mi><msub><mi>ρ</mi><mrow><mi>D</mi><mi>E</mi><mi>V</mi></mrow></msub></mrow></semantics></math></inline-formula>, with a constant <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mi>α</mi></semantics></math></inline-formula>. One of the problems revealed recently in cosmology is a so-called Hubble tension (HT), which is the difference between values of the present Hubble constant, measured by observation of the universe at redshift <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>z</mi><mo>≲</mo><mn>1</mn></mrow></semantics></math></inline-formula>, and by observations of a distant universe with CMB fluctuations originated at <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>z</mi><mo>∼</mo><mn>1100</mn></mrow></semantics></math></inline-formula>. In this paper we suggest that this discrepancy may be explained by deviation of the cosmological expansion from a standard Lambda-CDM model of a flat universe, due to the action of an additional variable component DEV. Taking into account the influence of DEV on the universe’s expansion, we find the value of <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mi>α</mi></semantics></math></inline-formula> that could remove the HT problem. In order to maintain the almost constant DEV/DM energy density ratio during the time interval at <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>z</mi><mo><</mo><mn>1100</mn></mrow></semantics></math></inline-formula>, we suggest the existence of a wide mass DM particle distribution.Gennady S. Bisnovatyi-KoganMDPI AGarticledark energydark matterHubble constantElementary particle physicsQC793-793.5ENUniverse, Vol 7, Iss 412, p 412 (2021)
institution	DOAJ
collection	DOAJ
language	EN
topic	dark energy dark matter Hubble constant Elementary particle physics QC793-793.5
spellingShingle	dark energy dark matter Hubble constant Elementary particle physics QC793-793.5 Gennady S. Bisnovatyi-Kogan Cosmological Model with Interconnection between Dark Energy and Matter
description	It is accepted in the present cosmology model that the scalar field, which is responsible for the inflation stage in the early universe, transforms completely into matter, and the accelerated universe expansion is presently governed by dark energy (DE), whose origin is not connected with the inflationary scalar field. We suppose here that dark matter (DM) has a common origin with a small variable component of dark energy (DEV). We suggest that DE may presently have two components, one of which is the Einstein constant <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mi mathvariant="normal">Λ</mi></semantics></math></inline-formula>, and another, smaller component DEV (<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi mathvariant="normal">Λ</mi><mi>V</mi></msub></semantics></math></inline-formula>) comes from the remnants of the scalar field responsible for inflation, which gave birth to the origin of presently existing matter. In this note we consider only the stages of the universe expansion after recombination, <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>z</mi><mo>≃</mo><mn>1100</mn></mrow></semantics></math></inline-formula>, when DM was the most abundant component of the matter, therefore we suggest for simplicity that a connection exists between DM and DEV so that the ratio of their densities remains constant over all the stages after recombination, <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><msub><mi>ρ</mi><mrow><mi>D</mi><mi>M</mi></mrow></msub><mo>=</mo><mi>α</mi><msub><mi>ρ</mi><mrow><mi>D</mi><mi>E</mi><mi>V</mi></mrow></msub></mrow></semantics></math></inline-formula>, with a constant <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mi>α</mi></semantics></math></inline-formula>. One of the problems revealed recently in cosmology is a so-called Hubble tension (HT), which is the difference between values of the present Hubble constant, measured by observation of the universe at redshift <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>z</mi><mo>≲</mo><mn>1</mn></mrow></semantics></math></inline-formula>, and by observations of a distant universe with CMB fluctuations originated at <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>z</mi><mo>∼</mo><mn>1100</mn></mrow></semantics></math></inline-formula>. In this paper we suggest that this discrepancy may be explained by deviation of the cosmological expansion from a standard Lambda-CDM model of a flat universe, due to the action of an additional variable component DEV. Taking into account the influence of DEV on the universe’s expansion, we find the value of <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mi>α</mi></semantics></math></inline-formula> that could remove the HT problem. In order to maintain the almost constant DEV/DM energy density ratio during the time interval at <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>z</mi><mo><</mo><mn>1100</mn></mrow></semantics></math></inline-formula>, we suggest the existence of a wide mass DM particle distribution.
format	article
author	Gennady S. Bisnovatyi-Kogan
author_facet	Gennady S. Bisnovatyi-Kogan
author_sort	Gennady S. Bisnovatyi-Kogan
title	Cosmological Model with Interconnection between Dark Energy and Matter
title_short	Cosmological Model with Interconnection between Dark Energy and Matter
title_full	Cosmological Model with Interconnection between Dark Energy and Matter
title_fullStr	Cosmological Model with Interconnection between Dark Energy and Matter
title_full_unstemmed	Cosmological Model with Interconnection between Dark Energy and Matter
title_sort	cosmological model with interconnection between dark energy and matter
publisher	MDPI AG
publishDate	2021
url	https://doaj.org/article/c94604087dfb4634838ff0355898e704
work_keys_str_mv	AT gennadysbisnovatyikogan cosmologicalmodelwithinterconnectionbetweendarkenergyandmatter
_version_	1718410242351431680

Cosmological Model with Interconnection between Dark Energy and Matter

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