Non-Canonical Dark Energy Parameter Evolution in a Canonical Quintessence Cosmology
This study considers the specific case of a flat, minimally coupled to gravity, quintessence cosmology with a dark energy quartic polynomial potential that has the same mathematical form as the Higgs potential. Previous work on this case determined that the scalar field is given by a simple expressi...
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2024-09-01
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| author | Rodger I. Thompson |
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| description | This study considers the specific case of a flat, minimally coupled to gravity, quintessence cosmology with a dark energy quartic polynomial potential that has the same mathematical form as the Higgs potential. Previous work on this case determined that the scalar field is given by a simple expression of the Lambert W function in terms of the easily observable scale factor. This expression provides analytic equations for the evolution of cosmological dark energy parameters as a function of the scale factor for all points on the Lambert W function principal branch. The Lambert W function is zero at a scale factor of zero that marks the big bang. The evolutionary equations beyond the big bang describe a canonical universe that is similar to <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mo>Λ</mo></semantics></math></inline-formula>CDM, making it an excellent dynamical template to compare with observational data. The portion of the W function principal before the big bang extends to the infinite pre-bang past. It describes a noncanonical universe with an initially very low mass density that contracts by rolling down the dark energy potential to a singularity, big bang, at the scale factor zero point. This provides a natural origin for the big bang. It also raises the possibility that the universe existed before the big bang and is far older, and that it was once far larger than its current size. The recent increasing interest in the possibility of a dynamical universe instead of <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mo>Λ</mo></semantics></math></inline-formula>CDM makes the exploration of the nature of such universes particularly relevant. |
| format | Article |
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| issn | 2218-1997 |
| language | English |
| publishDate | 2024-09-01 |
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| spelling | doaj-art-fb40ff230ce649aa8096d4e1af9b4ae42025-08-20T01:55:57ZengMDPI AGUniverse2218-19972024-09-0110935610.3390/universe10090356Non-Canonical Dark Energy Parameter Evolution in a Canonical Quintessence CosmologyRodger I. Thompson0Department of Astronomy and Steward Observatory, University of Arizona, Tucson, AZ 85721, USAThis study considers the specific case of a flat, minimally coupled to gravity, quintessence cosmology with a dark energy quartic polynomial potential that has the same mathematical form as the Higgs potential. Previous work on this case determined that the scalar field is given by a simple expression of the Lambert W function in terms of the easily observable scale factor. This expression provides analytic equations for the evolution of cosmological dark energy parameters as a function of the scale factor for all points on the Lambert W function principal branch. The Lambert W function is zero at a scale factor of zero that marks the big bang. The evolutionary equations beyond the big bang describe a canonical universe that is similar to <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mo>Λ</mo></semantics></math></inline-formula>CDM, making it an excellent dynamical template to compare with observational data. The portion of the W function principal before the big bang extends to the infinite pre-bang past. It describes a noncanonical universe with an initially very low mass density that contracts by rolling down the dark energy potential to a singularity, big bang, at the scale factor zero point. This provides a natural origin for the big bang. It also raises the possibility that the universe existed before the big bang and is far older, and that it was once far larger than its current size. The recent increasing interest in the possibility of a dynamical universe instead of <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mo>Λ</mo></semantics></math></inline-formula>CDM makes the exploration of the nature of such universes particularly relevant.https://www.mdpi.com/2218-1997/10/9/356cosmological constraintdark energytheoretical model |
| spellingShingle | Rodger I. Thompson Non-Canonical Dark Energy Parameter Evolution in a Canonical Quintessence Cosmology Universe cosmological constraint dark energy theoretical model |
| title | Non-Canonical Dark Energy Parameter Evolution in a Canonical Quintessence Cosmology |
| title_full | Non-Canonical Dark Energy Parameter Evolution in a Canonical Quintessence Cosmology |
| title_fullStr | Non-Canonical Dark Energy Parameter Evolution in a Canonical Quintessence Cosmology |
| title_full_unstemmed | Non-Canonical Dark Energy Parameter Evolution in a Canonical Quintessence Cosmology |
| title_short | Non-Canonical Dark Energy Parameter Evolution in a Canonical Quintessence Cosmology |
| title_sort | non canonical dark energy parameter evolution in a canonical quintessence cosmology |
| topic | cosmological constraint dark energy theoretical model |
| url | https://www.mdpi.com/2218-1997/10/9/356 |
| work_keys_str_mv | AT rodgerithompson noncanonicaldarkenergyparameterevolutioninacanonicalquintessencecosmology |