Dark Branes for Dark Matter
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arXiv
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| Auteurs principaux: | , , , |
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| Format: | Preprint |
| Publié: |
2024
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| _version_ | 1866911992050089984 |
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| author | Koutroulis, Fotis Megias, Eugenio Pokorski, Stefan Quiros, Mariano |
| author_facet | Koutroulis, Fotis Megias, Eugenio Pokorski, Stefan Quiros, Mariano |
| contents | We propose a setup for the origin of dark matter based on spacetime with a warped extra dimension and three branes: the Planck brane, the TeV brane, at a (few) TeV scale $ρ_T$, and a dark brane, at a (sub)-GeV scale $ρ_1\lesssim 100$ GeV $\llρ_T$. The Standard Model is localized in the TeV brane, thus solving the Higgs hierarchy problem, while the dark matter $χ$, a Dirac fermion with mass $m_χ<ρ_1$, is localized in the dark brane. The radion, with mass $m_r<m_χ$, interacts strongly ($\sim m_χ/ρ_1\sim\mathcal O(1)$) with dark matter and very weakly ($\sim m_{f}ρ_1/ρ_T^2\ll 1$) with the Standard Model matter $f$. The generic conflict between the bounds on its detection signatures and its proper relic abundance is avoided as dark matter annihilation is $p$-wave suppressed. The former is determined by its very weak interactions with the SM and the latter by its much stronger annihilation into radions. Therefore, there is a vast range in the Dark Matter's parameter space where the correct relic abundance is achieved consistently with the existing bounds. Moreover, for the dark brane with $ρ_1\lesssim 3$ GeV, a confinement/deconfinement first order phase transition, where the radion condensates, produces a stochastic gravitational waves background at the nanoHz frequencies, which can be identified with the signal detected by the Pulsar Timing Array (PTA) experiments. In the PTA window, for $0.15 \textrm{ GeV}\lesssim m_χ\lesssim 2$ GeV the relic abundance is reproduced and all constraints are satisfied. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2403_06276 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Dark Branes for Dark Matter Koutroulis, Fotis Megias, Eugenio Pokorski, Stefan Quiros, Mariano High Energy Physics - Phenomenology High Energy Astrophysical Phenomena General Relativity and Quantum Cosmology We propose a setup for the origin of dark matter based on spacetime with a warped extra dimension and three branes: the Planck brane, the TeV brane, at a (few) TeV scale $ρ_T$, and a dark brane, at a (sub)-GeV scale $ρ_1\lesssim 100$ GeV $\llρ_T$. The Standard Model is localized in the TeV brane, thus solving the Higgs hierarchy problem, while the dark matter $χ$, a Dirac fermion with mass $m_χ<ρ_1$, is localized in the dark brane. The radion, with mass $m_r<m_χ$, interacts strongly ($\sim m_χ/ρ_1\sim\mathcal O(1)$) with dark matter and very weakly ($\sim m_{f}ρ_1/ρ_T^2\ll 1$) with the Standard Model matter $f$. The generic conflict between the bounds on its detection signatures and its proper relic abundance is avoided as dark matter annihilation is $p$-wave suppressed. The former is determined by its very weak interactions with the SM and the latter by its much stronger annihilation into radions. Therefore, there is a vast range in the Dark Matter's parameter space where the correct relic abundance is achieved consistently with the existing bounds. Moreover, for the dark brane with $ρ_1\lesssim 3$ GeV, a confinement/deconfinement first order phase transition, where the radion condensates, produces a stochastic gravitational waves background at the nanoHz frequencies, which can be identified with the signal detected by the Pulsar Timing Array (PTA) experiments. In the PTA window, for $0.15 \textrm{ GeV}\lesssim m_χ\lesssim 2$ GeV the relic abundance is reproduced and all constraints are satisfied. |
| title | Dark Branes for Dark Matter |
| topic | High Energy Physics - Phenomenology High Energy Astrophysical Phenomena General Relativity and Quantum Cosmology |
| url | https://arxiv.org/abs/2403.06276 |