Primordial black hole formation in inflationary 
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-attractor models

Mahbub, Rafid

doi:10.1103/physrevd.101.023533

Cited by 56 publications

(42 citation statements)

References 65 publications

(119 reference statements)

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“…For example, the induced GWs from various inflationary models can be found in Refs. [100][101][102][103][104][105][106][107][108][109][110][111][112][113][114][115][116][117][118] and [62,116,119,120] in the context of Higgs inflation. In particular, the large induced GW counterpart to PBH as the totality of dark matter is studied in Refs.…”

Section: Induced Gws Historymentioning

confidence: 99%

Scalar Induced Gravitational Waves Review

2021

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We provide a review on the state-of-the-art of gravitational waves induced by primordial fluctuations, so-called induced gravitational waves. We present the intuitive physics behind induced gravitational waves and we revisit and unify the general analytical formulation. We then present general formulas in a compact form, ready to be applied. This review places emphasis on the open possibility that the primordial universe experienced a different expansion history than the often assumed radiation dominated cosmology. We hope that anyone interested in the topic will become aware of current advances in the cosmology of induced gravitational waves, as well as becoming familiar with the calculations behind.

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Section: Induced Gws Historymentioning

confidence: 99%

Scalar Induced Gravitational Waves Review

2021

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“…Depending on the re-entry horizon era, the mathematical formalisms applied to determine the mass fraction and the energy density of GWs will be different. Here, we discuss whether PBHs produce in the RD era or reheating epoch [88].…”

Section: Reheating Stagementioning

confidence: 99%

“…where w > −1/3. The number of e-folds throughout the reheating period is Ñreh ≡ ln (a reh /a end ) = [3(1 + w reh )] −1 ln (ρ end /ρ reh ), in which a reh shows the value of the scale factor at the end of reheating [47,88]. Also,…”

Section: Reheating Stagementioning

confidence: 99%

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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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“…Interestingly, the presence of such a pronounced dip in the spectrum is a universal feature, being virtually present in all single field models based on non-attractor evolution that are aiming to generate a sizeable peak in the power spectrum for producing PBH, say of order ∆P R /P R 10 7 (see e.g. [18][19][20][21][22][23][24][25]). As can be noticed from Figure 1, following the scales corresponding to the dip feature, the power spectrum grows with a spectral index that can be as large as n s − 1 = 4 [8] towards the peak 2 .…”

Section: 1mentioning

confidence: 99%