Reheating constraints on mutated hilltop inflation
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arXiv
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| Autores principales: | , , |
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| Formato: | Preprint |
| Publicado: |
2024
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| _version_ | 1866909311498715136 |
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| author | Yadav, Sudhava Gangal, Dhwani Venkataratnam, K. K. |
| author_facet | Yadav, Sudhava Gangal, Dhwani Venkataratnam, K. K. |
| contents | Future research studies of cosmic microwave background polarization seems likely to provide a more improved upper bound of $r \le 0.03$ on the tensor-to-scalar ratio(r). In our work, we have done the reheating study of mutated hilltop inflation(MHI), a model falling in the broad category of small field inflation. We have parameterized reheating in terms of various parameters like reheating duration $N_{\text{rh}}$, reheating temperature $T_{\text{rh}}$ and effective equation of state $\overline{ω}_{\text{rh}}$ using observationally viable values of scalar power spectrum amplitude $A_{\text{s}}$ and scalar spectral index $n_{\text{s}}$. In our study, working over a range of $\overline{ω}_{\text{rh}}$, we found that the MHI potential is well consistent with combined Planck and BK18 observations for $\overline{ω}_{\text{rh}} > 0$ within a particular range of model's parameter space and the lower values of the model parameter in MHI generate considerably smaller r compared to normal hilltop potential without any incompatibility of $n_s$ with observational data, making MHI a better choice in accordance to recent and future studies. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2401_09806 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Reheating constraints on mutated hilltop inflation Yadav, Sudhava Gangal, Dhwani Venkataratnam, K. K. Cosmology and Nongalactic Astrophysics Future research studies of cosmic microwave background polarization seems likely to provide a more improved upper bound of $r \le 0.03$ on the tensor-to-scalar ratio(r). In our work, we have done the reheating study of mutated hilltop inflation(MHI), a model falling in the broad category of small field inflation. We have parameterized reheating in terms of various parameters like reheating duration $N_{\text{rh}}$, reheating temperature $T_{\text{rh}}$ and effective equation of state $\overline{ω}_{\text{rh}}$ using observationally viable values of scalar power spectrum amplitude $A_{\text{s}}$ and scalar spectral index $n_{\text{s}}$. In our study, working over a range of $\overline{ω}_{\text{rh}}$, we found that the MHI potential is well consistent with combined Planck and BK18 observations for $\overline{ω}_{\text{rh}} > 0$ within a particular range of model's parameter space and the lower values of the model parameter in MHI generate considerably smaller r compared to normal hilltop potential without any incompatibility of $n_s$ with observational data, making MHI a better choice in accordance to recent and future studies. |
| title | Reheating constraints on mutated hilltop inflation |
| topic | Cosmology and Nongalactic Astrophysics |
| url | https://arxiv.org/abs/2401.09806 |