Violation of non-Gaussianity consistency relation in a single-field inflationary model
By M. H. Namjoo, H. Firouzjahi, Misao Sasaki. 2012
301 citations recorded by the source corpus.
In this paper we present a simple, toy model of single-field inflation in which the standard non-Gaussianity consistency condition is violated. In this model the curvature perturbations on super-horizon scales are not conserved and the decaying modes of perturbations are not negligible in the non-attractor phase. As a result a large local non-Gaussianity can be obtained in the squeezed limit which violates the standard non-Gaussianity consistency condition for the single-field models.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/0aef96c1c0365ab6639c5c3b1dcee79d308642d5
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Citations in the corpus
- Revisiting non-Gaussianity from non-attractor inflation models (2017, methodology): “For non-attractor inflation, one extra subtlety one should take care of is that the number of e-folds N does not only depend on the initial field value φ , but also on the initial field velocity π [17].”
- Steepest growth of the power spectrum and primordial black holes (2018, background): “This is despite the fact that one of the main reasons that USR inflation was initially considered interesting was that it appeared to generate local non-Gaussianity of order-unity amplitude [71], providing an exception to the statement that single-field inflation generates negligible local non-Gauss”
- Inflation, Cosmic Perturbations and Non-Gaussianities (2013, background): “However the non-Gaussianity becomes fNL ∼ 5/2, which is not only order one but also breaks the consistency relation of single field inflation [164, 165].”
- On primordial black holes from an inflection point (2017, background): “Finally, the ultra-slow-roll phase is characterised by two curvature modes: a constant and a growing one [14].”
- Primordial black holes from inflation and non-Gaussianity (2018, background): “The non-Gaussianity turns out to be completely local (δφ is basically a massless scalar field on the de Sitter background in the limit ≪ 1 and non-Gaussianity is generated after Hubble radius crossing) [59, 60, 63] 〈 ζ~k1ζ~k2ζ~k3 〉 = 3 · (2π)(3)δ((3))(~k1 + ~k2 + ~k3) [Pζ(k1)Pζ(k2) + two terms] .”
- Inflation with a constant rate of roll (2014, background): “Furthermore, the non-Gaussianity consistency relation for single field inflation can be violated [16].”