Impact of nonlinear overdensity statistics on primordial black hole abundance

Mahbub, Rafid

doi:10.1103/physrevd.102.023538

Cited by 10 publications

(12 citation statements)

References 40 publications

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“…If PBH formation is under investigation, then the P ζ obtained from σ = 5×10 −4 might be sufficient. But it is also known that PBH abundance depends on the choice of window functions [54,55] and whether one uses peaks theory or Press-Schechter [56,57]. This investigation is deferred to a future work.…”

Section: Discussion and Comparison With Slow-roll Noisementioning

confidence: 99%

Numerically modeling stochastic inflation in slow-roll and beyond

De,

Mahbub

2020

Preprint

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We present a complete numerical treatment of inflationary dynamics under the influence of stochastic corrections from sub-Hubble modes. We discuss how to exactly model the stochastic noise terms arising from the sub-Hubble quantum modes that give rise to the coarse-grained inflaton dynamics in the form of stochastic differential equations. The stochastic differential equations are solved event-by-event on a discrete time grid. We then compute the power spectrum of curvature perturbations that can be compared with the power spectrum computed in the traditional fashion using the Mukhanov-Sasaki equation by canonically quantizing the inflaton fluctuations. Our numerical procedure helps us to easily extend the formalism to ultra slow-roll inflation and study the possibility of primordial black hole formation.

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Section: Discussion and Comparison With Slow-roll Noisementioning

confidence: 99%

Numerically modeling stochastic inflation in slow-roll and beyond

De,

Mahbub

2020

Preprint

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“…The standard treatment of β(M ) is based on the Press-Schechter formalism [76] of the gravitational collapse that is used widely in large-scale structure studies [77]. In this formalism, β(M ) is given by the probability that the fractional overdensity δ ≡ δρ/ρ is above a certain threshold δ c for PBH formation [78,79]. For Gaussian primordial fluctuations, β(M ) is given by [80,81]:…”

Section: Pbh Formation and Abundancementioning

confidence: 99%

On Primordial Black Holes and secondary gravitational waves generated from inflation with solo/multi-bumpy potential

Zheng,

Shi,

Qiu

2021

Preprint

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It is well known that primordial black hole (PBH) can be generated in inflation process of the early universe, especially when the inflaton field has some non-trivial features that could break the slowroll condition. In this paper, we investigate a toy model of inflation with bumpy potential, which has one or several bumps. We found that potential with multi-bump can give rise to power spectra with multi-peaks in small-scale region, which can in turn predict the generation of primordial black holes in various mass ranges. We also consider the two possibilities of PBH formation by spherical collapse and elliptical collapse.

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“…Hitherto, numerous methodologies have been proposed to enhance the curvature power spectrum about seven order of magnitude on small scales relative to CMB scales. This aim could be achievable in Standard Model (SM) of inflation [28][29][30][31][32], modified gravity models [23][24][25], scalar-tensor theories [17][18][19][20][21][22] and non-canonical scalar field models [11][12][13][14] as well. Over and above the single field inflationary models, enhancement of the P R and production of PBHs in multi-field inflationary models could be achievable [33][34][35].…”

Section: Introductionmentioning

confidence: 99%

“…In the SM of inflation, the USR span to produce PBHs could be attained either by dint of an inflection point in the inflationary potential [28][29][30][31], or adding a correction term like a bump/dip to the base potential to reduce the velocity of the inflaton [16,32].…”

Section: Introductionmentioning

confidence: 99%

Primordial black holes ensued from exponential potential and coupling parameter in nonminimal derivative inflation model

Heydari

Karami

2022

J. Cosmol. Astropart. Phys.

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Here, Primordial Black Holes (PBHs) creation from exponential potential has been inquired, through gravitationally raised friction emanated from the nonminimal coupling between gravity and field derivative setup. Setting a two-parted exponential function of inflaton field as coupling parameter, and fine-tuning of four parameter Cases of our model, we could sufficiently slow down the inflaton owing to high friction during an ultra slow-roll phase. This empowers us to achieve enough enhancement in the amplitude of curvature perturbations power spectra, via numerical solving of Mukhanov-Sasaki equation. Thereafter, we illustrate the generation of four PBHs with disparate masses in RD era, corresponding to our four parameter Cases. Two specimens of these PBHs with stellar 𝒪(10)M ⊙ and earth 𝒪(10-6)M ⊙ masses can be appropriate to explicate the LIGO-VIRGO events, and the ultrashort-timescale microlensing events in OGLE data, respectively. Another two Cases of PBHs have asteroid masses around 𝒪(10-13)M ⊙ and 𝒪(10-15)M ⊙ with abundance of 96% and 95% of the Dark Matter (DM) content of the universe. Furthermore, we scrutinize the induced Gravitational Waves (GWs) ensued from PBHs production in our model. Subsequently, we elucidate that their contemporary density parameter spectra (ΩGW0 ) for all predicted Cases have acmes which lie in the sensitivity scopes of the GWs detectors, thereupon the verity of our conclusions can be verified in view of deduced data from these detectors. At length, our numerical outcomes exhibit a power-law behavior for the spectra of ΩGW0 with respect to frequency as ΩGW0 (f) ∼ (f/fc ) n in the proximity of acmes position. As well, in the infrared regime f ≪ fc , the log-reliant form of power index as n = 3 - 2/ln(fc /f) is attained.

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Impact of nonlinear overdensity statistics on primordial black hole abundance

Cited by 10 publications

References 40 publications

Numerically modeling stochastic inflation in slow-roll and beyond

Numerically modeling stochastic inflation in slow-roll and beyond

On Primordial Black Holes and secondary gravitational waves generated from inflation with solo/multi-bumpy potential

Primordial black holes ensued from exponential potential and coupling parameter in nonminimal derivative inflation model

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