de Sitter swampland conjecture in string field inflation
Abstract In this paper, we study a particular type of inflation by using non-local Friedman equations that are derived from the zero levels of string field theory and express a tachyonic action. Then, we challenge it by further refining de Sitter (dS) swampland conjecture (FRdSSC) monitoring. Theref...
| Main Authors: | , , , , |
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| Format: | Article |
| Language: | English |
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SpringerOpen
2023-07-01
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| Series: | European Physical Journal C: Particles and Fields |
| Online Access: | https://doi.org/10.1140/epjc/s10052-023-11822-2 |
| _version_ | 1797689014814244864 |
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| author | J. Sadeghi B. Pourhassan S. Noori Gashti İ. Sakallı M. R. Alipour |
| author_facet | J. Sadeghi B. Pourhassan S. Noori Gashti İ. Sakallı M. R. Alipour |
| author_sort | J. Sadeghi |
| collection | DOAJ |
| description | Abstract In this paper, we study a particular type of inflation by using non-local Friedman equations that are derived from the zero levels of string field theory and express a tachyonic action. Then, we challenge it by further refining de Sitter (dS) swampland conjecture (FRdSSC) monitoring. Therefore, we investigate some quantities, such as potential and Hubble parameters. We also consider slow-roll parameters to examine quantities such as the scalar spectrum index and the tensor-to-scalar ratio. Using straightforward calculations, we investigate this model from the swampland conjecture perspective in terms of the cosmological parameters, i.e., ( $$n_s$$ n s ), (r), and observable data such as Planck 2018, by constructing some structures such as $$(c_{1,2}-n_s)$$ ( c 1 , 2 - n s ) and $$(c_{1,2}-r_s)$$ ( c 1 , 2 - r s ) . Then, we make a new restriction for this conjecture as $$c_1^2c_2^2$$ c 1 2 c 2 2 and get a limit for this model in the range $$c<0.0942$$ c < 0.0942 . We find this inflationary model is strongly in tension with the dS swampland conjecture (dSSC), i.e., $$c_1=c_2 \ne {\mathcal {O}}(1)$$ c 1 = c 2 ≠ O ( 1 ) . So, we shall challenge it with the FRdSSC, which has some free parameters, viz., $$a,b>0$$ a , b > 0 , $$a+b=1$$ a + b = 1 , and $$q>2$$ q > 2 . By setting these parameters, we examine the compatibility of the mentioned conjecture with this inflationary model. Finally, we infer from this string field inflation (SFI) model that it satisfies the FRdSSC with the constraint of its free parameters a, b, and q. |
| first_indexed | 2024-03-12T01:40:52Z |
| format | Article |
| id | doaj.art-0fdb78b8821f497eb0ab9a614640cd76 |
| institution | Directory Open Access Journal |
| issn | 1434-6052 |
| language | English |
| last_indexed | 2024-03-12T01:40:52Z |
| publishDate | 2023-07-01 |
| publisher | SpringerOpen |
| record_format | Article |
| series | European Physical Journal C: Particles and Fields |
| spelling | doaj.art-0fdb78b8821f497eb0ab9a614640cd762023-09-10T11:24:24ZengSpringerOpenEuropean Physical Journal C: Particles and Fields1434-60522023-07-0183711110.1140/epjc/s10052-023-11822-2de Sitter swampland conjecture in string field inflationJ. Sadeghi0B. Pourhassan1S. Noori Gashti2İ. Sakallı3M. R. Alipour4Department of Physics, Faculty of Basic Sciences, University of MazandaranSchool of Physics, Damghan UniversitySchool of Physics, Damghan UniversityPhysics Department, Eastern Mediterranean UniversityDepartment of Physics, Faculty of Basic Sciences, University of MazandaranAbstract In this paper, we study a particular type of inflation by using non-local Friedman equations that are derived from the zero levels of string field theory and express a tachyonic action. Then, we challenge it by further refining de Sitter (dS) swampland conjecture (FRdSSC) monitoring. Therefore, we investigate some quantities, such as potential and Hubble parameters. We also consider slow-roll parameters to examine quantities such as the scalar spectrum index and the tensor-to-scalar ratio. Using straightforward calculations, we investigate this model from the swampland conjecture perspective in terms of the cosmological parameters, i.e., ( $$n_s$$ n s ), (r), and observable data such as Planck 2018, by constructing some structures such as $$(c_{1,2}-n_s)$$ ( c 1 , 2 - n s ) and $$(c_{1,2}-r_s)$$ ( c 1 , 2 - r s ) . Then, we make a new restriction for this conjecture as $$c_1^2c_2^2$$ c 1 2 c 2 2 and get a limit for this model in the range $$c<0.0942$$ c < 0.0942 . We find this inflationary model is strongly in tension with the dS swampland conjecture (dSSC), i.e., $$c_1=c_2 \ne {\mathcal {O}}(1)$$ c 1 = c 2 ≠ O ( 1 ) . So, we shall challenge it with the FRdSSC, which has some free parameters, viz., $$a,b>0$$ a , b > 0 , $$a+b=1$$ a + b = 1 , and $$q>2$$ q > 2 . By setting these parameters, we examine the compatibility of the mentioned conjecture with this inflationary model. Finally, we infer from this string field inflation (SFI) model that it satisfies the FRdSSC with the constraint of its free parameters a, b, and q.https://doi.org/10.1140/epjc/s10052-023-11822-2 |
| spellingShingle | J. Sadeghi B. Pourhassan S. Noori Gashti İ. Sakallı M. R. Alipour de Sitter swampland conjecture in string field inflation European Physical Journal C: Particles and Fields |
| title | de Sitter swampland conjecture in string field inflation |
| title_full | de Sitter swampland conjecture in string field inflation |
| title_fullStr | de Sitter swampland conjecture in string field inflation |
| title_full_unstemmed | de Sitter swampland conjecture in string field inflation |
| title_short | de Sitter swampland conjecture in string field inflation |
| title_sort | de sitter swampland conjecture in string field inflation |
| url | https://doi.org/10.1140/epjc/s10052-023-11822-2 |
| work_keys_str_mv | AT jsadeghi desitterswamplandconjectureinstringfieldinflation AT bpourhassan desitterswamplandconjectureinstringfieldinflation AT snoorigashti desitterswamplandconjectureinstringfieldinflation AT isakallı desitterswamplandconjectureinstringfieldinflation AT mralipour desitterswamplandconjectureinstringfieldinflation |