A case study of small field inflationary dynamics in the Einstein–Gauss–Bonnet framework in the light of <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline" id="d1e1469" altimg="si2.svg"><mml:mrow><mml:mi>G</mml:mi><mml:mi>W</mml:mi><mml:mn>170817</mml:mn></mml:mrow></mml:math>

Gangopadhyay, Mayukh R.; Khan, Hussain Ahmed; Yogesh, .

doi:10.1016/j.dark.2023.101177

Cited by 10 publications

(2 citation statements)

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“…We consider the Einstein-GB action as follows (Guo & Dominik 2010;Jiang et al 2013;Koh et al 2014;Gao 2020;Odintsov et al 2020aOdintsov et al , 2020bPozdeeva et al 2020;Rashidi & Nozari 2020;Azizi et al 2022;Khan 2022;Shahraeini et al 2022;Gangopadhyay & Khan 2023;Nojiri et al 2023;Odintsov et al 2023Odintsov et al , 2023Nojiri & Odintsov 2024):…”

Section: Gauss-bonnet Inflationary Modelmentioning

confidence: 99%

“…where a is the scale factor. The Friedmann equations and the equation of motion can be derived by taking variation of the action (1) with respect to the metric g μ ν and the scalar field f, respectively as follows (Guo & Dominik 2010;Jiang et al 2013;Koh et al 2014;Gao 2020;Odintsov et al 2020aOdintsov et al , 2020bPozdeeva et al 2020;Khan 2022;Gangopadhyay & Khan 2023;Nojiri et al 2023;Odintsov et al 2023Odintsov et al , 2023:…”

Section: Gauss-bonnet Inflationary Modelmentioning

confidence: 99%

See 1 more Smart Citation

Primordial Black Holes in Scalar Field Inflation Coupled to the Gauss–Bonnet Term with Fractional Power-law Potentials

Ashrafzadeh,

Karami

2024

ApJ

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In this study, we investigate the formation of primordial black holes (PBHs) in a scalar field inflationary model coupled to the Gauss–Bonnet term with fractional power-law potentials. The coupling function enhances the curvature perturbations, then results in the generation of PBHs and detectable secondary gravitational waves (GWs). We identify three separate sets of parameters for the potential functions of the form ϕ 1/3, ϕ 2/5, and ϕ 2/3. By adjusting the model parameters, we decelerate the inflaton during the ultra-slow-roll phase and enhance curvature perturbations. Our calculations predict the formation of PBHs with masses of O ( 10 ) M ⊙ , which are compatible with LIGO-Virgo observational data. Additionally, we find PBHs with masses around O ( 10 − 6 ) M ⊙ and O ( 10 − 5 ) M ⊙ , which can explain ultra-short-timescale microlensing events in OGLE data. Furthermore, our proposed mechanism could lead to the formation of PBHs in mass scales around O ( 10 − 14 ) M ⊙ and O ( 10 − 13 ) M ⊙ , contributing to approximately 99% of the dark matter in the Universe. We also study the production of secondary GWs in our model. In all cases of the model, the density parameter of secondary GWs Ω GW 0 exhibits peaks that intersect the sensitivity curves of GW detectors, providing a means to verify our findings using data of these detectors. Our numerical results demonstrate a power-law behavior for the spectra of Ω GW 0 with respect to frequency, given by Ω GW 0 ( f ) ∼ ( f / f c ) n . Additionally, in the infrared regime where f ≪ f c , the power index takes a log-dependent form, specifically n = 3 − 2 / ln ( f c / f ) .

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