Early Dark Energy During Big Bang Nucleosynthesis
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arXiv
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| Format: | Preprint |
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2024
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| _version_ | 1866909390369456128 |
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| author | McKeen, David Omar, Afif |
| author_facet | McKeen, David Omar, Afif |
| contents | We study the impact of an early dark energy component (EDE) present during big bang nucleosynthesis (BBN) on the elemental abundances of deuterium D/H, and helium $Y_p$, as well as the effective relativistic degrees of freedom $N_{\rm eff}$. We consider a simple model of EDE that is constant up to a critical time. After this critical time, the EDE transitions into either a radiation component that interacts with the electromagnetic plasma, a dark radiation component that is uncoupled from the plasma, or kination that is also uncoupled. We use measured values of the abundances and $N_{\rm eff}$ as determined by CMB observations to establish limits on the input parameters of this EDE model. In addition, we explore how those parameters are correlated with BBN inputs; the baryon to photon ratio $η_b$, neutron lifetime $τ_n$, and number of neutrinos $N_ν$. Finally, we study whether this setup can alleviate the tension introduced by recent measurements of the primordial helium abundance. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2407_03508 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Early Dark Energy During Big Bang Nucleosynthesis McKeen, David Omar, Afif High Energy Physics - Phenomenology Cosmology and Nongalactic Astrophysics We study the impact of an early dark energy component (EDE) present during big bang nucleosynthesis (BBN) on the elemental abundances of deuterium D/H, and helium $Y_p$, as well as the effective relativistic degrees of freedom $N_{\rm eff}$. We consider a simple model of EDE that is constant up to a critical time. After this critical time, the EDE transitions into either a radiation component that interacts with the electromagnetic plasma, a dark radiation component that is uncoupled from the plasma, or kination that is also uncoupled. We use measured values of the abundances and $N_{\rm eff}$ as determined by CMB observations to establish limits on the input parameters of this EDE model. In addition, we explore how those parameters are correlated with BBN inputs; the baryon to photon ratio $η_b$, neutron lifetime $τ_n$, and number of neutrinos $N_ν$. Finally, we study whether this setup can alleviate the tension introduced by recent measurements of the primordial helium abundance. |
| title | Early Dark Energy During Big Bang Nucleosynthesis |
| topic | High Energy Physics - Phenomenology Cosmology and Nongalactic Astrophysics |
| url | https://arxiv.org/abs/2407.03508 |