Primordial black holes from string inflation

Cicoli, Michele; Diaz, Victor Alfonzo; Pedro, Francisco Manuel Soares Verissimo Gil

doi:10.1088/1475-7516/2018/06/034

Cited by 143 publications

(205 citation statements)

References 100 publications

(218 reference statements)

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“…In particular, there are a plethora of inflationary scenarios able to generate PBHs in the late Universe, see e.g., Refs. [80][81][82][83][84][85][86][87][88][89][90][91][92][93]. In this paper we concentrate on this scenario of PBHs generated by primordial curvature (C) perturbations, CPBHs.…”

Section: Introductionmentioning

confidence: 99%

From primordial black holes abundance to primordial curvature power spectrum (and back)

Kalaja

Bellomo

Bartolo

et al. 2019

J. Cosmol. Astropart. Phys.

105

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In the model where Primordial Black Holes (PBHs) form from large primordial curvature (C) perturbations, i.e., CPBHs, constraints on PBH abundance provide in principle constraints on the primordial curvature power spectrum. This connection however depends necessarily on the details of PBH formation mechanism. In this paper we provide, for the first time, constraints on the primordial curvature power spectrum from the latest limits on PBH abundance, taking into account all the steps from gravitational collapse in real space to PBH formation. In particular, we use results from numerical relativity simulations and peak theory to study the conditions for PBH formation for a range of perturbation shapes, including nonlinearities, perturbation profile and a careful treatment of smoothing and filtering scales. We then obtain updated PBH formation conditions and translate that into primordial spectrum constraints for a wide range of shapes and abundances. These updated constraints cover a range of scales not probed by other cosmological observables. Our results show that the correct and accurate modelling of non-linearities, filtering and typical perturbation profile, is crucial for deriving meaningful cosmological implications.

show abstract

Section: Introductionmentioning

confidence: 99%

From primordial black holes abundance to primordial curvature power spectrum (and back)

Kalaja

Bellomo

Bartolo

et al. 2019

J. Cosmol. Astropart. Phys.

105

View full text Add to dashboard Cite

show abstract

“…This happens when the large curvature fluctuations at small scales produced during inflation, reenter the Hubble horizon after inflation. The large curvature fluctuations at scales much smaller than the CMB scale can be produced in various models, for instance, a period of ultra-slow-roll [3][4][5][6][7][8][9][10], sound speed resonance [11] and an early dust-like stage [12,13] etc.. The amplification of density fluctuations can also be caused by subhorizon nonlinear dynamics such as phase transition [14][15][16][17][18] and preheating [19][20][21][22].…”

Section: Introductionmentioning

confidence: 99%

Primordial black holes from cosmic domain walls

2020

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We investigate the formation of primordial black holes (PBHs) from the collapse of spherically symmetric domain wall bubbles, which spontaneously nucleate via quantum tunneling during inflation. Since the tension of domain walls changes with time and so domain walls nucleate in a short time interval, the mass function of PBHs in general has a spike-like structure. In contrast to models in which PBHs produced from overdense regions, our model avoids the uncertainties of PBHs production mechanism. PBHs from domain walls with mass around 10 20 g may constitute all dark matter, those with mass around 10 34 g can explain the merger events of binary black holes detected by LIGO.

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“…1 Such an amplification is possible in models which exhibit certain peculiarities in the inflaton potential. Amplification of the curvature power spectrum has been shown to be achievable in various models such as multi-field inflation models like hybrid inflation [9,10], double inflation [11] and a collection of models where the inflaton potential contains a plateau-like region exhibiting ultra slow-roll (USR) dynamics such as (i) string theory inspired models [12,13] (ii) critical Higgs inflation [14] (iii) radiative plateau inflation [15] (iv) MSSM inflation [16] and (v) inflationary α-attractors [17] among others.…”

Section: Introductionmentioning

confidence: 99%

Primordial black hole formation in inflationary α -attractor models

Mahbub

2020

Phys. Rev. D

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The formation of primordial black holes is studied using superconformal inflationary α-attractors. An inflaton potential is constructed with a plateau-like region which brings about the onset of an ultra slow-roll region where the required enhancement in the curvature power spectrum takes place. This is accomplished by carefully finetuning the parameters in the potential. For the parameter sets, the amount of observable inflation is such that the curvature perturbation P R peaks at ∼ 10 14 Mpc −1 , producing PBHs in the mass window 10 16 g ≤ M ≤ 10 18 g. The reheating period after inflation is taken into account to determine whether or not PBH formation takes place in such a phase. Finally, the spectrum of second order gravitational waves, that can arise due to the curvature perturbation enhancement, is calculated.

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Primordial black holes from string inflation

Cited by 143 publications

References 100 publications

From primordial black holes abundance to primordial curvature power spectrum (and back)

From primordial black holes abundance to primordial curvature power spectrum (and back)

Primordial black holes from cosmic domain walls

Primordial black hole formation in inflationary α -attractor models

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