Primordial black holes generated by the non-minimal spectator field

Meng, De-Shuang; Yuan, Chen; Huang, Qingguo

doi:10.1007/s11433-022-2095-5

Cited by 36 publications

(11 citation statements)

References 204 publications

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“…2) gives the quadratic potential, namely V cur (χ) ≃ 1 2 m 2 χ χ 2 , which is studied in refs. [20,21]. The homogeneous EoMs derived from the action (2.1) with the spatially flat Friedmann-Lemaître-Robertson-Walker metric, ds 2 = −dt 2 +a 2 (t)δ ij dx i dx j , are given by…”

Section: Master Perturbation Equationsmentioning

confidence: 99%

“…for the axion-like potential (2.2). The background (2.5) and perturbation (2.13) equations do not share the same form as the case for the quadratic curvaton's JCAP08(2023)041 potential [20,21], and one cannot apply the fixed ratio δχ/χ to simplify the analysis except for the small-field limit χ ≪ f a . Deep inside the horizon k ≫ aH, the Bunch-Davies (BD) vacuum can be utilized to establish the initial condition for δχ k ,…”

Section: Enhancement From a Non-trivial Field Metricmentioning

confidence: 99%

“…[20] and studied further by the following ref. [21] with three specific forms of field metric, including the Gaussian-like, rectangular and oscillating dips. However, some JCAP08(2023)041 discrepancies were observed in the curvaton power spectrum at the end of inflation, for which the underlying reason is unclear.…”

Section: Introductionmentioning

confidence: 99%

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Growth of curvature perturbations for PBH formation & detectable GWs in non-minimal curvaton scenario revisited

Chen,

Ghoshal,

Lalak

et al. 2023

J. Cosmol. Astropart. Phys.

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We revisit the growth of curvature perturbations in non-minimal curvaton scenario with a non-trivial field metric λ(ϕ) where ϕ is an inflaton field, and incorporate the effect from the non-uniform onset of curvaton's oscillation in terms of an axion-like potential. The field metric λ(ϕ) plays a central role in the enhancement of curvaton field perturbation δχ, serving as an effective friction term which can be either positive or negative, depending on the first derivative λ ,ϕ . Our analysis reveals that δχ undergoes the superhorizon growth when the condition η eff ≡ -2 √2ϵ M Pl λ ,ϕ /λ < -3 is satisfied. This is analogous to the mechanism responsible for the amplification of curvature perturbations in the context of ultra-slow-roll inflation, namely the growing modes dominate curvature perturbations. As a case study, we examine the impact of a Gaussian dip in λ(ϕ) and conduct a thorough investigation of both the analytical and numerical aspects of the inflationary dynamics. Our findings indicate that the enhancement of curvaton perturbations during inflation is not solely determined by the depth of the dip in λ(ϕ). Rather, the first derivative λ ,ϕ also plays a significant role, a feature that has not been previously highlighted in the literature. Utilizing the δ𝒩 formalism, we derive analytical expressions for both the final curvature power spectrum and the non-linear parameter f NL in terms of an axion-like curvaton's potential leading to the non-uniform curvaton's oscillation. Additionally, the resulting primordial black hole abundance and scalar-induced gravitational waves are calculated, which provide observational windows for PBHs.

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Section: Master Perturbation Equationsmentioning

confidence: 99%

Section: Enhancement From a Non-trivial Field Metricmentioning

confidence: 99%

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Growth of curvature perturbations for PBH formation & detectable GWs in non-minimal curvaton scenario revisited

Chen,

Ghoshal,

Lalak

et al. 2023

J. Cosmol. Astropart. Phys.

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“…It contains no leading Gaussian term, unlike in scenarios with a non-vanishing curvaton mean value |⟨χ⟩| ≫ H (a specific initial condition during inflation) which have been studied previously in the PBH context e.g. in [47][48][49][50][51]. We use the δN formalism to obtain the full non-linear solution for ζ as a function of χ and, following [63], include only the monopole term of the spherical harmonics series of χ(x) when considering fluctuations relevant for PBHs.…”

Section: Jcap11(2023)006mentioning

confidence: 99%

“…In this work, we focus on the curvaton scenario [42][43][44][45][46]. Several authors have already investigated PBH formation in curvaton models [47][48][49][50][51] and other spectator scenarios [52][53][54][55][56][57] where the curvature perturbation can acquire non-Gaussian contributions. The effect of this non-Gaussianity is typically treated perturbatively, using the parameters f NL etc.…”

Section: Introductionmentioning

confidence: 99%

Primordial black holes from a curvaton scenario with strongly non-Gaussian perturbations

Gow,

Miranda,

Nurmi

2023

J. Cosmol. Astropart. Phys.

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We investigate the production of primordial black holes (PBHs) in a mixed inflaton-curvaton scenario with a quadratic curvaton potential, assuming the curvaton is in de Sitter equilibrium during inflation with 〈χ〉 = 0. In this setup, the curvature perturbation sourced by the curvaton is strongly non-Gaussian, containing no leading Gaussian term. We show that for m 2/H 2 ≳ 0.3, the curvaton contribution to the spectrum of primordial perturbations on CMB scales can be kept negligible but on small scales the curvaton can source PBHs. In particular, PBHs in the asteroid mass range 10-16 M ⊙ ≲ M ≲ 10-10 M ⊙ with an abundance reaching F PBH = 1 can be produced when the inflationary Hubble scale H ≳ 1012 GeV and the curvaton decay occurs in the window from slightly before the electroweak transition to around the QCD transition.

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Implications for the supermassive black hole binaries from the NANOGrav 15-year data set

Bi,

Wu,

Chen

et al. 2023

Sci. China Phys. Mech. Astron.

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Primordial black holes generated by the non-minimal spectator field

Cited by 36 publications

References 204 publications

Growth of curvature perturbations for PBH formation & detectable GWs in non-minimal curvaton scenario revisited

Growth of curvature perturbations for PBH formation & detectable GWs in non-minimal curvaton scenario revisited

Primordial black holes from a curvaton scenario with strongly non-Gaussian perturbations

Implications for the supermassive black hole binaries from the NANOGrav 15-year data set

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