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| Formato: | Preprint |
| Publicado: |
2024
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| Acceso en línea: | https://arxiv.org/abs/2409.16403 |
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| author | Khodam-Mohammadi, A. |
| author_facet | Khodam-Mohammadi, A. |
| contents | This study explores the interaction between non-extensive entropic FLRW cosmology and the power-law inflationary model, with a focus on the overlap between the scalar spectral index `$n_s$' and the tensor-to-scalar ratio `$r$'. Based on a conjecture that non-extensive entropy alters the energy-momentum content of the cosmic fluid, the analysis examines how these overlaps shift with different model parameters and compares the findings to those from Bekenstein-Hawking (BH) entropic cosmology. The study highlights the impact of Tsallis, Rényi, and Sharma-Mittal entropies, uncovering a significant correlation between `$n_s$' and `$r$' that suggests a deeper connection in power-law inflationary dynamics. The results demonstrate that non-extensive entropies not only enable viable inflation with a graceful exit but also address limitations inherent in the standard BH entropic framework, emphasizing the importance of precise parameter estimation. Specifically, Tsallis entropy allows for power-law inflation with $n = 1$ to $n = 2$ in alignment with Planck 2018 data. Moreover, the $α$ parameter in Rényi and Sharma-Mittal entropy models must be extremely small ($α\leq 10^{-8}$ in Planck mass units) to achieve successful power-law inflation with an e-folding number around 55-65, suggesting a unified thermodynamic perspective in cosmological studies. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2409_16403 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Non-Extensive Entropy and Power-Law Inflation: Implications for Observations Khodam-Mohammadi, A. General Relativity and Quantum Cosmology This study explores the interaction between non-extensive entropic FLRW cosmology and the power-law inflationary model, with a focus on the overlap between the scalar spectral index `$n_s$' and the tensor-to-scalar ratio `$r$'. Based on a conjecture that non-extensive entropy alters the energy-momentum content of the cosmic fluid, the analysis examines how these overlaps shift with different model parameters and compares the findings to those from Bekenstein-Hawking (BH) entropic cosmology. The study highlights the impact of Tsallis, Rényi, and Sharma-Mittal entropies, uncovering a significant correlation between `$n_s$' and `$r$' that suggests a deeper connection in power-law inflationary dynamics. The results demonstrate that non-extensive entropies not only enable viable inflation with a graceful exit but also address limitations inherent in the standard BH entropic framework, emphasizing the importance of precise parameter estimation. Specifically, Tsallis entropy allows for power-law inflation with $n = 1$ to $n = 2$ in alignment with Planck 2018 data. Moreover, the $α$ parameter in Rényi and Sharma-Mittal entropy models must be extremely small ($α\leq 10^{-8}$ in Planck mass units) to achieve successful power-law inflation with an e-folding number around 55-65, suggesting a unified thermodynamic perspective in cosmological studies. |
| title | Non-Extensive Entropy and Power-Law Inflation: Implications for Observations |
| topic | General Relativity and Quantum Cosmology |
| url | https://arxiv.org/abs/2409.16403 |