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

Heydari, Soma; Karami, K.

doi:10.1088/1475-7516/2022/03/033

Cited by 26 publications

(8 citation statements)

References 163 publications

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“…An alternative is to keep the potential simple and featureless but modify the gravitational component of the action beyond a simple non-minimal coupling. Examples of these models include F (R) gravity [114], Dirac-Born-Infeld inflation [70], a non-minimal derivative coupling between the inflaton and gravity [78,85,102,107], Gauss-Bonnet inflation [103], warm inflation [80,96,157], axion inflation with gauge fields [88], G-or k-inflation [92,98,101]. Typically, in these models, the enhancement of the power spectrum arises due to its modified expression, which, apart from the potential, also depends on the extra non-minimal functions of the scalar field.…”

Section: Jcap03(2023)013mentioning

confidence: 99%

Anatomy of single-field inflationary models for primordial black holes

Καράμ

Koivunen

Tomberg

et al. 2023

J. Cosmol. Astropart. Phys.

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We construct an analytically solvable simplified model that captures the essential features for primordial black hole (PBH) production in most models of single-field inflation. The construction makes use of the Wands duality between the constant-roll (or slow-roll) and the preceding ultra-slow-roll phases and can be realized by a simple inflaton potential of two joined parabolas. Within this framework, it is possible to formulate explicit inflationary scenarios consistent with the CMB observations and copious production of PBHs of arbitrary mass. We quantify the variability of the shape of the peak in the curvature power spectrum in different inflationary scenarios and discuss its implications for probing PBHs with scalar-induced gravitational wave backgrounds. We find that the COBE/Firas μ-distortion constraints exclude the production of PBHs heavier than 104 M ⊙ in single-field inflation.

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Section: Jcap03(2023)013mentioning

confidence: 99%

Anatomy of single-field inflationary models for primordial black holes

Καράμ

Koivunen

Tomberg

et al. 2023

J. Cosmol. Astropart. Phys.

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“…We expect that in these models the equilateral non-Gaussianity presents a substantial enhancement too, that can be examined in future investigations. But there are some models, such as the non-minimal derivative [33][34][35][36] and k/G [37][38][39][40][41][42][43][44][45] inflationary scenarios, in which the variation of the scalar power spectrum is rather mild over all scales, and so we expect that these models do not show a large enhancement in the equilateral non-Gaussianity and it remains of order f equil NL 1 in all scales. This point also may be verified by further examinations in the future.…”

Section: Calculation Of Non-gaussianitymentioning

confidence: 96%

Non-Gaussianity and secondary gravitational waves from primordial black holes production in $$\alpha $$-attractor inflation

2022

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We study the non-Gaussianity and secondary Gravitational Waves (GWs) in the process of the Primordial Black Holes (PBHs) production from inflation. In our work, we focus on the $$\alpha $$ α -attractor inflation model in which a tiny bump in the inflaton potential enhances the amplitude of the curvature perturbations at some scales and consequently leads to the PBHs production with different mass scales. We implement the computational code BINGO which calculates the non-Gaussianity parameter in different triangle configurations. Our examination implies that in this setup, the non-Gaussianity gets amplified significantly in the equilateral shape around the scales in which the power spectrum of the scalar perturbations undergoes a sharp declination. The imprints of these non-Gaussianities can be probed in the scales corresponding to the BBN and $$\mu $$ μ -distortion events, or in smaller scales, and detection of such signatures in the future observations may confirm the idea of our model for the generation of PBHs or rule it out. Moreover, we investigate the secondary GWs in this framework and show that in our model, the peak of the present fractional energy density is obtained as $$\Omega _{\mathrm{GW0}} \sim 10^{-8}$$ Ω GW 0 ∼ 10 - 8 at different frequencies which depends on the model parameters. These results lie well within the sensitivity region of some GWs detectors at some frequencies, and therefore the observational compatibility of our model can be evaluated by the forthcoming data from these detectors. We further provide some estimations for the tilts of the induced GWs spectrum in the different intervals of frequency, and demonstrate that the spectrum obeys the power-law relation $$\Omega _{\mathrm{GW0}}\sim f^{n}$$ Ω GW 0 ∼ f n in those frequency bands.

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“…PBHs with mass O(10 −5 )M ⊙ and abundance O(10 −2 ), can be located in the permitted span of OGLE data [27,51] and they can be suitable to expound the ultrashort-timescale microlensing events in this zone. Due to the fact that, There is no constraint on PBHs abundance in the mass scope of O(10 −16 − 10 −11 )M ⊙ , the located PBHs in this zone could be contemplated as an appropriate candidate for the DM content in its totality [13][14][15][16][17][18][19][20][21].…”

Section: Introductionmentioning

confidence: 99%

Primordial black holes in non-canonical scalar field inflation driven by quartic potential in the presence of bump

Heydari,

Karami

2024

J. Cosmol. Astropart. Phys.

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Here, generation of Primordial Black Holes (PBHs) from quartic potential in the presence of a tiny bump in non-canonical inflationary model has been inquired. It is demonstrated that, a viable inflationary era can be driven through the quartic potential in non-canonical framework with a power-law Lagrangian density. Furthermore, setting a suitable function of inflaton field as a correction term (like a bump) to the quartic potential, causes the inflaton to slow down for a while. In such a short time span, the amplitude of the scalar perturbations power spectrum on small scales grows up sufficiently versus CMB scales. In addition to the bump feature, the enhancing effect of the α parameter of the Lagrangian on the amplitude of the scalar power spectrum has been shown. Fine tuning of three parameter Cases of the model results in generating of three Cases of PBHs. In addition, we investigate the secondary Gravitational Waves (GWs) produced during generation of PBHs and show that their contemporary density parameter spectra (ΩGW0 ) can be tracked down by GWs detectors.

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

Cited by 26 publications

References 163 publications

Anatomy of single-field inflationary models for primordial black holes

Anatomy of single-field inflationary models for primordial black holes

Non-Gaussianity and secondary gravitational waves from primordial black holes production in $$\alpha $$-attractor inflation

Primordial black holes in non-canonical scalar field inflation driven by quartic potential in the presence of bump

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