Primordial black holes from α-attractors

By I. Dalianis, A. Kehagias, G. Tringas. Journal of Cosmology and Astroparticle Physics, 2018

220 citations recorded by the source corpus.

We consider primordial black hole (PBH) production in inflationary α-attractors. We discuss two classes of models, namely models with a minimal polynomial superpotential as well as modulated chaotic ones that admit PBHs. We find that a significant amplification of the curvature power spectrum 𝒫R can be realized in this class of models with a moderate tuning of the potential parameters. We consistently examine the PBH formation during radiation and additionally during reheating eras where the background pressure is negligible. It is shown that basic features of the curvature power spectrum are explicitly related with the postinflationary cosmic evolution and that the PBH mass and abundance expressions are accordingly modified. PBHs in the mass range 10−16−10−14 M⊙ can form with a cosmologically relevant abundance for a power spectrum peak 𝒫R ∼ 10−2 and large reheating temperature and, furthermore, for a moderate peak 𝒫R ∼ 10−5 and reheating temperature Trh∼ 107 GeV, characteristic of the position of the power spectrum peak. Regarding the CMB observables, the α-attractor models utilized here to generate PBH in the low-mass region predict in general a smaller ns and larger r and αs parameter values compared to the conventional inflationary α-attractor models.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/dc2348e0e187746c771b837cd05b417b3badfe31

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Citations in the corpus

Generating PBHs and small-scale GWs in two-field models of inflation (2020, background): “This can be achieved in single-field inflation scenarios by using a local feature in the inflaton potential like a rapid change of its amplitude or a break in its first derivative [7–9], an inflection point [10–18] or a tiny bump superimposed on it [19, 20], non-trivial inflaton sound speed [21–23]1”
Primordial black holes from a tiny bump/dip in the inflaton potential (2019, background): “See [70, 71] for PBH formation in near inflection point models constructed from α-attractor potentials.”