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| Main Authors: | , , , , , |
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| Format: | Preprint |
| Published: |
2025
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| Subjects: | |
| Online Access: | https://arxiv.org/abs/2509.15360 |
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| _version_ | 1866912703385174016 |
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| author | Zambrano, Jordan Agama, Miguel Garzón, Marcos Bramer-Escamilla, Werner Rojas, Clara Vargas, Teófilo |
| author_facet | Zambrano, Jordan Agama, Miguel Garzón, Marcos Bramer-Escamilla, Werner Rojas, Clara Vargas, Teófilo |
| contents | In this work, we solved the scalar and tensor perturbation equations numerically and using the improved uniform approximation method together with the third-order phase-integral method, for the $α$-attractor inflationary model. This inflationary model has become very important because it allows us to describe the initial accelerated expansion of the universe in the inflationary epoch, and the current accelerated expansion with the same potential that depends on one scalar field $φ$. Once the equations for the scalar and tensor power spectra are found, we calculate the observables: the scalar-to-tensor ratio $r$, and the scalar spectral index $n_S$, concluding that semiclassical methods give excellent results compared to numerical integration. We also compare both observables in the $α$-attractor and the Starobinsky inflationary model. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2509_15360 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Quintessential inflation studied through Semiclassical Methods Zambrano, Jordan Agama, Miguel Garzón, Marcos Bramer-Escamilla, Werner Rojas, Clara Vargas, Teófilo Cosmology and Nongalactic Astrophysics In this work, we solved the scalar and tensor perturbation equations numerically and using the improved uniform approximation method together with the third-order phase-integral method, for the $α$-attractor inflationary model. This inflationary model has become very important because it allows us to describe the initial accelerated expansion of the universe in the inflationary epoch, and the current accelerated expansion with the same potential that depends on one scalar field $φ$. Once the equations for the scalar and tensor power spectra are found, we calculate the observables: the scalar-to-tensor ratio $r$, and the scalar spectral index $n_S$, concluding that semiclassical methods give excellent results compared to numerical integration. We also compare both observables in the $α$-attractor and the Starobinsky inflationary model. |
| title | Quintessential inflation studied through Semiclassical Methods |
| topic | Cosmology and Nongalactic Astrophysics |
| url | https://arxiv.org/abs/2509.15360 |