Production of Primordial Black Holes in Improved E-Models of Inflation
E-type <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mi>α</mi></semantics></math></inline-formula>-attractor models of single-field inflation were generalized further in order to accom...
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MDPI AG
2023-06-01
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| Series: | Universe |
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| Online Access: | https://www.mdpi.com/2218-1997/9/6/294 |
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| author | Daniel Frolovsky Sergei V. Ketov |
| author_facet | Daniel Frolovsky Sergei V. Ketov |
| author_sort | Daniel Frolovsky |
| collection | DOAJ |
| description | E-type <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mi>α</mi></semantics></math></inline-formula>-attractor models of single-field inflation were generalized further in order to accommodate production of primordial black holes (PBHs) via adding a near-inflection point to the inflaton scalar potential at smaller scales, in good agreement with measurements of cosmic microwave background (CMB) radiation. A minimal number of new parameters were used but their fine-tuning was maximized in order to increase the possible masses of PBHs formed during an ultra-slow-roll phase, leading to a large enhancement in the power spectrum of scalar (curvature) perturbations by 6 or 7 orders of magnitude against the power spectrum of perturbations observed in CMB. It was found that extreme fine-tuning of the parameters in our models can lead to the formation of moon-sized PBHs, with masses of up to <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mn>10</mn><mn>26</mn></msup></semantics></math></inline-formula> g, still in agreement with CMB observations. Quantum corrections are known to lead to the perturbative upper bound on the amplitude of large scalar perturbations responsible for PBH production. The quantum (one-loop) corrections in our models were found to be suppressed by one order of magnitude for PBHs with masses of approximately <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mn>10</mn><mn>19</mn></msup></semantics></math></inline-formula> g, which may form the whole dark matter in the Universe. |
| first_indexed | 2024-03-11T01:51:13Z |
| format | Article |
| id | doaj.art-9c47a741fb634cb68b2aca83dc866c89 |
| institution | Directory Open Access Journal |
| issn | 2218-1997 |
| language | English |
| last_indexed | 2024-03-11T01:51:13Z |
| publishDate | 2023-06-01 |
| publisher | MDPI AG |
| record_format | Article |
| series | Universe |
| spelling | doaj.art-9c47a741fb634cb68b2aca83dc866c892023-11-18T12:57:23ZengMDPI AGUniverse2218-19972023-06-019629410.3390/universe9060294Production of Primordial Black Holes in Improved E-Models of InflationDaniel Frolovsky0Sergei V. Ketov1Interdisciplinary Research Laboratory, Tomsk State University, Tomsk 634050, RussiaInterdisciplinary Research Laboratory, Tomsk State University, Tomsk 634050, RussiaE-type <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mi>α</mi></semantics></math></inline-formula>-attractor models of single-field inflation were generalized further in order to accommodate production of primordial black holes (PBHs) via adding a near-inflection point to the inflaton scalar potential at smaller scales, in good agreement with measurements of cosmic microwave background (CMB) radiation. A minimal number of new parameters were used but their fine-tuning was maximized in order to increase the possible masses of PBHs formed during an ultra-slow-roll phase, leading to a large enhancement in the power spectrum of scalar (curvature) perturbations by 6 or 7 orders of magnitude against the power spectrum of perturbations observed in CMB. It was found that extreme fine-tuning of the parameters in our models can lead to the formation of moon-sized PBHs, with masses of up to <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mn>10</mn><mn>26</mn></msup></semantics></math></inline-formula> g, still in agreement with CMB observations. Quantum corrections are known to lead to the perturbative upper bound on the amplitude of large scalar perturbations responsible for PBH production. The quantum (one-loop) corrections in our models were found to be suppressed by one order of magnitude for PBHs with masses of approximately <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mn>10</mn><mn>19</mn></msup></semantics></math></inline-formula> g, which may form the whole dark matter in the Universe.https://www.mdpi.com/2218-1997/9/6/294inflationprimordial black holes |
| spellingShingle | Daniel Frolovsky Sergei V. Ketov Production of Primordial Black Holes in Improved E-Models of Inflation Universe inflation primordial black holes |
| title | Production of Primordial Black Holes in Improved E-Models of Inflation |
| title_full | Production of Primordial Black Holes in Improved E-Models of Inflation |
| title_fullStr | Production of Primordial Black Holes in Improved E-Models of Inflation |
| title_full_unstemmed | Production of Primordial Black Holes in Improved E-Models of Inflation |
| title_short | Production of Primordial Black Holes in Improved E-Models of Inflation |
| title_sort | production of primordial black holes in improved e models of inflation |
| topic | inflation primordial black holes |
| url | https://www.mdpi.com/2218-1997/9/6/294 |
| work_keys_str_mv | AT danielfrolovsky productionofprimordialblackholesinimprovedemodelsofinflation AT sergeivketov productionofprimordialblackholesinimprovedemodelsofinflation |