Cosmic inflation in the context of κ-deformed theories
This paper addresses a new inflationary scenario driven by a slowly-rolling homogeneous scalar field, assuming a generalized potential inspired by Kaniadakis' κ-deformed theory, defined as expκ(x)=(1+κ2x2+κx)1/κ. We show that this kind of potential can arise in the context of brane cosmology,...
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| Main Authors: | , , |
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| Format: | Article |
| Language: | English |
| Published: |
Elsevier
2025-08-01
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| Series: | Nuclear Physics B |
| Subjects: | |
| Online Access: | http://www.sciencedirect.com/science/article/pii/S0550321325001300 |
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| Summary: | This paper addresses a new inflationary scenario driven by a slowly-rolling homogeneous scalar field, assuming a generalized potential inspired by Kaniadakis' κ-deformed theory, defined as expκ(x)=(1+κ2x2+κx)1/κ. We show that this kind of potential can arise in the context of brane cosmology, where the field describing the size of the extra-dimension, so-called radion, is interpreted as the inflaton. Within the slow-roll approximation, we obtain the main predictions of the model and compare them with current data from cosmic microwave background and large-scale structure observations. We show that this single scalar field model admits a wider set of solutions than usual exponential scenarios and predicts acceptable values for the spectral index, running of the spectral index, and tensor-to-scalar ratio for the remaining number of e-folds lying in the interval N=55±5 and an energy scale on which λ≥2. In particular, our findings suggest that the κ-parameter value depends on the analysis. For instance, the ns−κ and αs−ns planes point out to κ≲0.2, while the fNLlocal−κ analysis discards κ values very close to zero. Finally, combining these analyses, we conclude that 0.02≲κ≲0.2. |
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| ISSN: | 0550-3213 |