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Testing a Two Field Inflation Beyond the Slow-Roll Approximation
Cosmology and Nongalactic Astrophysics · Submitted 3 May 2016
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Our study shows that for some ranges of the DBI parameter, the model is consistent with observation and it is also possible to have large non-Gaussianity which would be observable by future improvements in experiments.
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The abstract, sentence by sentence
We consider a model of two-field inflation, containing an ordinary scalar field and a DBI field. We work beyond the slow-roll approximation, but we assume a separable Hubble parameter. We then derive the form of potential in this framework and study the spectrum of the primordial perturbations in details. We also study the amplitude of the non-Gaussianity of the primordial perturbations both in equilateral and orthogonal configurations in this setup. We test the model with recent observational data and find some constraints on the model parameters. Our study shows that for some ranges of the DBI parameter, the model is consistent with observation and it is also possible to have large non-Gaussianity which would be observable by future improvements in experiments.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We consider a model of two-field inflation, containing an ordinary scalar field and a DBI field. | method 0.49 | 0.52 | 0.02 | asserted 0.94 |
| s1 | We work beyond the slow-roll approximation, but we assume a separable Hubble parameter. | method 0.86 | 0.93 | 0.02 | asserted 0.98 |
| s2 | We then derive the form of potential in this framework and study the spectrum of the primordial perturbations in details. | contribution 0.62 | 0.96 | 0.04 | asserted 0.96 |
| s3 | We also study the amplitude of the non-Gaussianity of the primordial perturbations both in equilateral and orthogonal configurations in this setup. | contribution 0.93 | 0.96 | 0.04 | asserted 0.96 |
| s4 | We test the model with recent observational data and find some constraints on the model parameters. | result 0.43 | 0.97 | 0.08 | asserted 1.00 |
| s5 | Our study shows that for some ranges of the DBI parameter, the model is consistent with observation and it is also possible to have large non-Gaussianity which would be observable by future improvements in experiments. | result 0.72 | 0.96 | 0.92 | hedged possibility 0.91 |
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The paper
Original abstract
We consider a model of two-field inflation, containing an ordinary scalar field and a DBI field. We work beyond the slow-roll approximation, but we assume a separable Hubble parameter. We then derive the form of potential in this framework and study the spectrum of the primordial perturbations in details. We also study the amplitude of the non-Gaussianity of the primordial perturbations both in equilateral and orthogonal configurations in this setup. We test the model with recent observational data and find some constraints on the model parameters. Our study shows that for some ranges of the DBI parameter, the model is consistent with observation and it is also possible to have large non-Gaussianity which would be observable by future improvements in experiments.
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What it cites · 6 sentences without a confident label
Uses the method or tool of 3 papers
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In this regard, we follow [ref] and introduce a shape $S_*^equil$ as [equation] Moreover, we define another shape which is exactly orthogonal to $S_*^equil$, as follows [equation] where $β≃1.1967996$.
Lecture notes on non-Gaussianity · Nonlinear Perturbations and Non-Gaussianity · 0.96
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In other words, since slow-roll condition can be temporarily violated during inflation (for example if fields start to decay during inflation as in staggered/cascade inflation [ref] , if a bump in the potential is encountered, and it is necessarily violated at the end of inflation and during reheating), we go beyond this approximation and our strategy is based on the first order Hamilton-Jacobi formalism developed by Salopek and Bond in Ref. [ref] , which allows us to express inflationary parameters in the model, without having to focus on a slow-roll regime (one can see [ref] for application of this formalism to the single-field case).
Exposition to Staggered Multi-Field Inflation · Introduction · 0.96
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In other words, since slow-roll condition can be temporarily violated during inflation (for example if fields start to decay during inflation as in staggered/cascade inflation [ref] , if a bump in the potential is encountered, and it is necessarily violated at the end of inflation and during reheating), we go beyond this approximation and our strategy is based on the first order Hamilton-Jacobi formalism developed by Salopek and Bond in Ref. [ref] , which allows us to express inflationary parameters in the model, without having to focus on a slow-roll regime (one can see [ref] for application of this formalism to the single-field case).
Power Spectrum and Signatures for Cascade Inflation · Introduction · 0.96
Uses data or values from 3 papers
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Recently, the Planck collaboration released the constraints $r < 0.099$ and $n_s=0.9652 ±0.0047$ from Planck TT, TE, EE+low P+WP data [ref] .
Planck 2015 results. XVII. Constraints on primordial non-Gaussianity · Introduction · 0.95
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Recently, the Planck collaboration released the constraints $r < 0.099$ and $n_s=0.9652 ±0.0047$ from Planck TT, TE, EE+low P+WP data [ref] .
Planck 2015 results. XX. Constraints on inflation · Introduction · 0.95
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Recently, the Planck collaboration released the constraints $r < 0.099$ and $n_s=0.9652 ±0.0047$ from Planck TT, TE, EE+low P+WP data [ref] .
Planck 2015 results. XIII. Cosmological parameters · Introduction · 0.95
Cites as background 2 papers
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Moreover, during inflation, the vacuum fluctuation of light scalar fields grow into super-Hubble density perturbations which are believed to be the origin of the structure formation in the universe [ref] .
Particle Physics and Inflationary Cosmology · Introduction · 0.99
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Moreover, during inflation, the vacuum fluctuation of light scalar fields grow into super-Hubble density perturbations which are believed to be the origin of the structure formation in the universe [ref] .
Inflation and the Theory of Cosmological Perturbations · Introduction · 0.99
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