Reheating after swampland conjecture
Abstract The evolution of the universe started from a hot and dense Big Bang point. Temperature fluctuation map of cosmic microwave background (CMB) radiation and initial seeds of large scale structures (LSS) are explained by an inflationary period in a very early time. Inflaton as quanta of the inf...
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SpringerOpen
2020-01-01
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| Series: | Journal of High Energy Physics |
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| Online Access: | https://doi.org/10.1007/JHEP01(2020)092 |
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| author | Vahid Kamali |
| author_facet | Vahid Kamali |
| author_sort | Vahid Kamali |
| collection | DOAJ |
| description | Abstract The evolution of the universe started from a hot and dense Big Bang point. Temperature fluctuation map of cosmic microwave background (CMB) radiation and initial seeds of large scale structures (LSS) are explained by an inflationary period in a very early time. Inflaton as quanta of the inflation field is responsible for the accelerated expansion of the universe. Potentials of the self-interacting single field models are constrained by observational data as well as quantum gravity. Some forms of the potential are rolled out by data of Planck satellite and some of them by quantum gravity constraints. In the standard model of inflation or cold inflation firstly universe expands where the inflaton rolls the nearly flat part of the potential and in the second part, the universe reheats where the inflaton oscillates around the minimum of the potential which leads to thermalized radiation dominated universe. String theory as the best model of quantum gravity forbids the oscillation around the minimum of the potential during the thermalized epoch of the reheating. But in the warm model of inflation thermalization happens during the accelerated expansion of the universe where the inflaton rolls nearly steep potential and the universe will be radiation dominated without any separated reheating epoch. |
| format | Article |
| id | doaj-art-fcf4f2adfb49424ca407d33ef9516290 |
| institution | Kabale University |
| issn | 1029-8479 |
| language | English |
| publishDate | 2020-01-01 |
| publisher | SpringerOpen |
| record_format | Article |
| series | Journal of High Energy Physics |
| spelling | doaj-art-fcf4f2adfb49424ca407d33ef95162902025-01-26T12:11:35ZengSpringerOpenJournal of High Energy Physics1029-84792020-01-012020111010.1007/JHEP01(2020)092Reheating after swampland conjectureVahid Kamali0Department of Physics, McGill UniversityAbstract The evolution of the universe started from a hot and dense Big Bang point. Temperature fluctuation map of cosmic microwave background (CMB) radiation and initial seeds of large scale structures (LSS) are explained by an inflationary period in a very early time. Inflaton as quanta of the inflation field is responsible for the accelerated expansion of the universe. Potentials of the self-interacting single field models are constrained by observational data as well as quantum gravity. Some forms of the potential are rolled out by data of Planck satellite and some of them by quantum gravity constraints. In the standard model of inflation or cold inflation firstly universe expands where the inflaton rolls the nearly flat part of the potential and in the second part, the universe reheats where the inflaton oscillates around the minimum of the potential which leads to thermalized radiation dominated universe. String theory as the best model of quantum gravity forbids the oscillation around the minimum of the potential during the thermalized epoch of the reheating. But in the warm model of inflation thermalization happens during the accelerated expansion of the universe where the inflaton rolls nearly steep potential and the universe will be radiation dominated without any separated reheating epoch.https://doi.org/10.1007/JHEP01(2020)092Cosmology of Theories beyond the SMEffective Field Theories |
| spellingShingle | Vahid Kamali Reheating after swampland conjecture Journal of High Energy Physics Cosmology of Theories beyond the SM Effective Field Theories |
| title | Reheating after swampland conjecture |
| title_full | Reheating after swampland conjecture |
| title_fullStr | Reheating after swampland conjecture |
| title_full_unstemmed | Reheating after swampland conjecture |
| title_short | Reheating after swampland conjecture |
| title_sort | reheating after swampland conjecture |
| topic | Cosmology of Theories beyond the SM Effective Field Theories |
| url | https://doi.org/10.1007/JHEP01(2020)092 |
| work_keys_str_mv | AT vahidkamali reheatingafterswamplandconjecture |