Inflationary and Gravitational Wave Signatures of Small Primordial Black Holes as Dark Matter
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arXiv
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| Natura: | Preprint |
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2024
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| _version_ | 1866913574089129984 |
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| author | Barker, Will Gladwyn, Benjamin Zell, Sebastian |
| author_facet | Barker, Will Gladwyn, Benjamin Zell, Sebastian |
| contents | Mounting evidence suggests that the semi-classical description of a black hole breaks down at the latest after losing an O(1) fraction of its mass. As a result, effects such as memory burden can slow down evaporation so that small primordial black holes (PBHs), in particular those in the mass range 10^6 g to 10^9 g, become viable dark matter candidates. In this paper, we investigate the production of PBHs from a prototype model of polynomial inflation with a non-minimal coupling to gravity. We show that a sufficiently small PBH mass alleviates any tension with CMB observations. Moreover, we develop efficient numerical procedures to identify model parameters and evolve Mukhanov-Sasaki modes to place bounds on the scalar-induced stochastic gravitational wave (GW) background. Whilst we identify some prospects for observation with future GW detectors, our results highlight the need to develop new experiments for high-frequency GW detection in the ~kHz to ~MHz range. Finally, we demonstrate that previously-used ansätze for modelling the power spectrum only yield a reliable approximation for the GW signal if some input from inflation is used. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2410_11948 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Inflationary and Gravitational Wave Signatures of Small Primordial Black Holes as Dark Matter Barker, Will Gladwyn, Benjamin Zell, Sebastian Cosmology and Nongalactic Astrophysics General Relativity and Quantum Cosmology High Energy Physics - Phenomenology High Energy Physics - Theory Mounting evidence suggests that the semi-classical description of a black hole breaks down at the latest after losing an O(1) fraction of its mass. As a result, effects such as memory burden can slow down evaporation so that small primordial black holes (PBHs), in particular those in the mass range 10^6 g to 10^9 g, become viable dark matter candidates. In this paper, we investigate the production of PBHs from a prototype model of polynomial inflation with a non-minimal coupling to gravity. We show that a sufficiently small PBH mass alleviates any tension with CMB observations. Moreover, we develop efficient numerical procedures to identify model parameters and evolve Mukhanov-Sasaki modes to place bounds on the scalar-induced stochastic gravitational wave (GW) background. Whilst we identify some prospects for observation with future GW detectors, our results highlight the need to develop new experiments for high-frequency GW detection in the ~kHz to ~MHz range. Finally, we demonstrate that previously-used ansätze for modelling the power spectrum only yield a reliable approximation for the GW signal if some input from inflation is used. |
| title | Inflationary and Gravitational Wave Signatures of Small Primordial Black Holes as Dark Matter |
| topic | Cosmology and Nongalactic Astrophysics General Relativity and Quantum Cosmology High Energy Physics - Phenomenology High Energy Physics - Theory |
| url | https://arxiv.org/abs/2410.11948 |