Inflationary and Gravitational Wave Signatures of Small Primordial Black Holes as Dark Matter
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...
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| creator | Barker, Will Gladwyn, Benjamin Zell, Sebastian |
| description | 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 ans\"atze for modelling the power spectrum only yield a
reliable approximation for the GW signal if some input from inflation is used. |
| doi_str_mv | 10.48550/arxiv.2410.11948 |
| format | Article |
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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 ans\"atze for modelling the power spectrum only yield a
reliable approximation for the GW signal if some input from inflation is used.</description><identifier>DOI: 10.48550/arxiv.2410.11948</identifier><language>eng</language><subject>Physics - Cosmology and Nongalactic Astrophysics ; Physics - General Relativity and Quantum Cosmology ; Physics - High Energy Physics - Phenomenology ; Physics - High Energy Physics - Theory</subject><creationdate>2024-10</creationdate><rights>http://arxiv.org/licenses/nonexclusive-distrib/1.0</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,776,881</link.rule.ids><linktorsrc>$$Uhttps://arxiv.org/abs/2410.11948$$EView_record_in_Cornell_University$$FView_record_in_$$GCornell_University$$Hfree_for_read</linktorsrc><backlink>$$Uhttps://doi.org/10.48550/arXiv.2410.11948$$DView paper in arXiv$$Hfree_for_read</backlink></links><search><creatorcontrib>Barker, Will</creatorcontrib><creatorcontrib>Gladwyn, Benjamin</creatorcontrib><creatorcontrib>Zell, Sebastian</creatorcontrib><title>Inflationary and Gravitational Wave Signatures of Small Primordial Black Holes as Dark Matter</title><description>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 ans\"atze for modelling the power spectrum only yield a
reliable approximation for the GW signal if some input from inflation is used.</description><subject>Physics - Cosmology and Nongalactic Astrophysics</subject><subject>Physics - General Relativity and Quantum Cosmology</subject><subject>Physics - High Energy Physics - Phenomenology</subject><subject>Physics - High Energy Physics - Theory</subject><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2024</creationdate><recordtype>article</recordtype><sourceid>GOX</sourceid><recordid>eNpjYJA0NNAzsTA1NdBPLKrILNMzMgEKGBpamlhwMsR65qXlJJZk5uclFlUqJOalKLgXJZZllkCEchTCE8tSFYIz0_MSS0qLUosV8tMUgnMTc3IUAooyc_OLUjKBapxyEpOzFTzyc4DyicUKLolF2Qq-iSUlqUU8DKxpiTnFqbxQmptB3s01xNlDF-yQ-AKgGUBr40EOigc7yJiwCgCAmkEX</recordid><startdate>20241015</startdate><enddate>20241015</enddate><creator>Barker, Will</creator><creator>Gladwyn, Benjamin</creator><creator>Zell, Sebastian</creator><scope>GOX</scope></search><sort><creationdate>20241015</creationdate><title>Inflationary and Gravitational Wave Signatures of Small Primordial Black Holes as Dark Matter</title><author>Barker, Will ; Gladwyn, Benjamin ; Zell, Sebastian</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-arxiv_primary_2410_119483</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2024</creationdate><topic>Physics - Cosmology and Nongalactic Astrophysics</topic><topic>Physics - General Relativity and Quantum Cosmology</topic><topic>Physics - High Energy Physics - Phenomenology</topic><topic>Physics - High Energy Physics - Theory</topic><toplevel>online_resources</toplevel><creatorcontrib>Barker, Will</creatorcontrib><creatorcontrib>Gladwyn, Benjamin</creatorcontrib><creatorcontrib>Zell, Sebastian</creatorcontrib><collection>arXiv.org</collection></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Barker, Will</au><au>Gladwyn, Benjamin</au><au>Zell, Sebastian</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Inflationary and Gravitational Wave Signatures of Small Primordial Black Holes as Dark Matter</atitle><date>2024-10-15</date><risdate>2024</risdate><abstract>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 ans\"atze for modelling the power spectrum only yield a
reliable approximation for the GW signal if some input from inflation is used.</abstract><doi>10.48550/arxiv.2410.11948</doi><oa>free_for_read</oa></addata></record> |
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| subjects | Physics - Cosmology and Nongalactic Astrophysics Physics - General Relativity and Quantum Cosmology Physics - High Energy Physics - Phenomenology Physics - High Energy Physics - Theory |
| title | Inflationary and Gravitational Wave Signatures of Small Primordial Black Holes as Dark Matter |
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