Gravitational waves from double-inflection-point inflation

Summary Primordial black holes (PBHs) might form from the collapse of over-densed regions generated by large scalar curvature perturbations in the radiation dominated era. Despite decades of various independent observations, the nature of dark matter (DM) remains highly puzzling. Recently, PBH DM have aroused interest since they provide an attracting explanation to the merger events of binary black holes discovered by LIGO/VIRGO and may play an important role on DM. During the formation of PBH, gravitational waves will be sourced by linear scalar perturbations at second-order, known as the scalar induced gravitational waves (SIGWs), which provides a new way to hunt for PBH DM. This topic review mainly focuses on the physics about SIGWs accompanying the formation of PBH DM.

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“…(2017a) ; Di and Gong (2018) ; Ando et al. (2018b , 2018c) ; Xu et al. (2020) ; Özsoy and Tasinato (2020) ; Gao and Yang (2019) ; Lin et al.…”

Section: Scalar Induced Gravitational Wavesmentioning

confidence: 99%

A topic review on probing primordial black hole dark matter with scalar induced gravitational waves

Yuan

Huang

2021

iScience

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“…The induced GWs can produce together with PBHs at the horizon re-entry of the primordial density perturbations [59][60][61][62][63][64][65][66][67][68][69][70][71][72][73][74]. The induced GWs can be tested by the GWs observatory like LISA [96].…”

Section: Induced Gravitational Wavesmentioning

confidence: 99%

“…Furthermore, the PBHs formation is followed by the generation of the induced gravitational waves (GWs), when the primordial curvature perturbations enhance significantly [59][60][61][62][63][64][65][66][67][68][69][70][71][72][73][74]. In other words, after the horizon re-entry, the collapse of the overdense regions can generate large metric perturbations besides PBHs.…”

Section: Introductionmentioning

confidence: 99%

Primordial black holes formation in the inflationary model with field-dependent kinetic term for quartic and natural potentials

Solbi

Karami

2021

Eur. Phys. J. C

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Within the framework of inflationary model with field-dependent kinetic term for quartic and natural potentials, we investigate generation of the primordial black holes (PBHs) and induced gravitational waves (GWs). In this setup, we consider a kinetic function as $$G(\phi )=g_I(\phi )\big (1+g_{II}(\phi )\big )$$ G ( ϕ ) = g I ( ϕ ) ( 1 + g II ( ϕ ) ) and show that in the presence of first term $$g_I(\phi )$$ g I ( ϕ ) both quartic and natural potentials, in contrast to the standard model of inflation, can be consistent, with the 68% CL of Planck observations. Besides, the second term $$g_{II}(\phi )$$ g II ( ϕ ) can cause a significant enhancement in the primordial curvature perturbations at the small scales which results the PBHs formation. For the both potentials, we obtain an enhancement in the scalar power spectrum at the scales $$k\sim 10^{12}~{\mathrm{Mpc}}^{-1}$$ k ∼ 10 12 Mpc - 1 , $$10^{8}~{\mathrm{Mpc}}^{-1}$$ 10 8 Mpc - 1 , and $$10^{5}~{\mathrm{Mpc}}^{-1}$$ 10 5 Mpc - 1 , which causes PBHs production in mass scales around $$10^{-13}M_{\odot }$$ 10 - 13 M ⊙ , $$10^{-5}M_{\odot }$$ 10 - 5 M ⊙ , and $$10 M_{\odot }$$ 10 M ⊙ , respectively. Observational constraints confirm that PBHs with a mass scale of $$10^{-13}M_{\odot }$$ 10 - 13 M ⊙ can constitute the total of dark matter in the universe. Furthermore, we estimate the energy density parameter of induced GWs which can be examined by the observation. Also we conclude that it can be parametrized as a power-law function $$\Omega _{\mathrm{GW}}\sim (f/f_c)^n$$ Ω GW ∼ ( f / f c ) n , where the power index equals $$n=3-2/\ln (f_c/f)$$ n = 3 - 2 / ln ( f c / f ) in the infrared limit $$f\ll f_{c}$$ f ≪ f c .

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“…Thus it is different from the models with only one peak, which can only be detected in one frequency range. So the double peak models can be distinguished from other single peak models [16][17][18][19][98][99][100].…”

Section: Energy Spectrum Of the Induced Gwsmentioning

confidence: 99%

“…In most of the inflationary models, the induced second-order GW is generically negligible compared to the first-order GWs. However, if the power spectrum of scalar perturbations is enhanced at small scales, the second-order GWs can be sizable or even larger than the first-order one [10][11][12][13][14][15][16][17][18][19][20][21][22].…”

Section: Introductionmentioning

confidence: 99%

Double peaks of gravitational wave spectrum induced from inflection point inflation

Gao

Yang

2021

Eur. Phys. J. C

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We investigate the possibility of inducing the gravitational waves (GWs) with double peak energy spectrum from primordial scalar perturbations in inflationary models with three inflection points. Here the inflection points can be generated from a polynomial potential or generated from a Higgs-like $$\phi ^4$$ ϕ 4 potential with the running of quartic coupling. In such models, the inflection point at large scales predicts the scalar spectral index and tensor-to-scalar ratio to be consistent with current CMB constraints, and the other two inflection points generate two large peaks in the scalar power spectrum at small scales, which can induce GWs with a double peak energy spectrum. We find that for some choices of the parameters the double peak spectrum can be detected by future GW detectors, and one of the peaks around $$f\simeq 10^{-9}{-}10^{-8}$$ f ≃ 10 - 9 - 10 - 8 Hz can also explain the recent NANOGrav signal. Moreover, the peaks of the power spectrum allow for the generation of primordial black holes, which accounts for a significant fraction of dark matter.

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Gravitational waves from double-inflection-point inflation

Cited by 80 publications

References 75 publications

A topic review on probing primordial black hole dark matter with scalar induced gravitational waves

A topic review on probing primordial black hole dark matter with scalar induced gravitational waves

Primordial black holes formation in the inflationary model with field-dependent kinetic term for quartic and natural potentials

Double peaks of gravitational wave spectrum induced from inflection point inflation

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