Inflationary and gravitational wave signatures of small primordial black holes as dark matter

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F68378271%3A_____%2F25%3A00637378" target="_blank" >RIV/68378271:_____/25:00637378 - isvavai.cz</a>

Výsledek na webu

<a href="https://doi.org/10.1103/4hrv-zfch" target="_blank" >https://doi.org/10.1103/4hrv-zfch</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1103/4hrv-zfch" target="_blank" >10.1103/4hrv-zfch</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Inflationary and gravitational wave signatures of small primordial black holes as dark matter

Popis výsledku v původním jazyce

Mounting evidence suggests that the semiclassical 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 106  g to 109  g, become viable dark matter candidates. In this paper, we investigate the production of PBHs from a prototype model of polynomial inflation with a nonminimal coupling to gravity. We show that a sufficiently small PBH mass alleviates any tension with cosmic microwave background 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. While 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 modeling the power spectrum only yield a reliable approximation for the GW signal if some input from inflation is used.

Název v anglickém jazyce

Inflationary and gravitational wave signatures of small primordial black holes as dark matter

Popis výsledku anglicky

Mounting evidence suggests that the semiclassical 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 106  g to 109  g, become viable dark matter candidates. In this paper, we investigate the production of PBHs from a prototype model of polynomial inflation with a nonminimal coupling to gravity. We show that a sufficiently small PBH mass alleviates any tension with cosmic microwave background 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. While 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 modeling the power spectrum only yield a reliable approximation for the GW signal if some input from inflation is used.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

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OECD FORD obor

10303 - Particles and field physics

Projekt

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Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2025

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Physical Review D

ISSN

2470-0010

e-ISSN

2470-0029

Svazek periodika

111

Číslo periodika v rámci svazku

12

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

22

Strana od-do

123033

Kód UT WoS článku

001519372100001

EID výsledku v databázi Scopus

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