Constraints on<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mi>α</mml:mi></mml:mrow></mml:math>-attractor inflation and reheating

Ueno, Yoshiki; Yamamoto, Kazuhiro

doi:10.1103/physrevd.93.083524

Cited by 104 publications

(90 citation statements)

References 44 publications

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“…The general properties of the reheating stage of α attractors have been very well studied by Ueno and Yamamoto in Ref. [15]. In Fig.…”

Section: Numerical Results and Discussionmentioning

confidence: 99%

“…After that, the inflaton field falls in the minimum of the potential V (ϕ), acquires a mass m ϕ , oscillates, and decays producing the relativistic degrees of freedom of radiationdominated plasma. This reheating phase can be modeled using an effective cosmic fluid described in terms of an equation-of-state parameter w reh [13][14][15]. The first model of reheating was proposed in [2], in a relatively simple setting where the field coherently oscillates around the minimum of a quadratic potential ∼ m 2 ϕ 2 .…”

Section: Reheating and Equation Of Statementioning

confidence: 99%

“…[14]) and to α-attractor models by Ueno and Yamamoto in Ref. [15]. Our analysis is also devoted to extract further possible constraints on the reheating phase in fiber inflation models given by the next generation of CMB polarization and Gravitational Waves (GW) experiments [21][22][23][24][25][26].…”

Section: Reheating and Equation Of Statementioning

confidence: 99%

“…The scalar field is subjected to a potential V (ϕ) that in the slowroll phase can drive an accelerated expansion of the Universe, with a typical duration of N * ∼ 60 e-folds. Nevertheless, several features of the inflationary physics are still elusive, and one of these is represented by the reheating phase in which the energy stored in the inflaton field is converted to thermal radiation, giving rise to the early radiation-dominated epoch of the standard hot big bang model [2][3][4][5][6][7][8][9][10][11][12][13][14][15]. The reheating is a fundamental stage of the Universe evolution and its details affect and constrain the range of several observables, for instance n s and r. Moreover, it is strongly model dependent and can be highly non-trivial, due to the nonlinear and nonperturbative processes involved.…”

Section: Introductionmentioning

confidence: 99%

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Fiber inflation and reheating

2017

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We present constraints on the reheating era within the string Fiber Inflation scenario, in terms of the effective equation-of-state parameter of the reheating fluid, w reh . The results of the analysis, completely independent on the details of the inflaton physics around the vacuum, illustrate the behavior of the number of e-foldings during the reheating stage, N reh , and of the final reheating temperature, T reh , as functions of the scalar spectral index, ns. We analyze our results with respect to the current bounds given by the PLANCK mission data and to upcoming cosmological experiments. We find that large values of the equation-of-state parameter (w reh > 1/3) are particularly favored as the scalar spectral index is of the order of ns ∼ 0.9680, with a σn s ∼ 0.002 error. Moreover, we compare the behavior of the general reheating functions N reh and T reh in the fiber Inflation scenario with the one extracted by the class of the α-attractor models with α = 2. We find that the corresponding reheating curves are very similar in the two cases.

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“…The general properties of the reheating stage of α attractors have been very well studied by Ueno and Yamamoto in Ref. [15]. In Fig.…”

Section: Numerical Results and Discussionmentioning

confidence: 99%

Section: Reheating and Equation Of Statementioning

confidence: 99%

Section: Reheating and Equation Of Statementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Fiber inflation and reheating

2017

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“…The energy density of the reheating epoch has the following relation with the temperature of this epoch [74,76] …”

Section: Reheatingmentioning

confidence: 99%

Perturbation, non-Gaussianity, and reheating in a Gauss-Bonnet α -attractor model

Nozari

Rashidi

2017

Phys. Rev. D

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Motivated by α-attractor models, in this paper we consider a Gauss-Bonnet inflation with an E-model-type of potential. We consider the Gauss-Bonnet coupling function to be the same as the E-model potential. In the small α limit we obtain an attractor at r = 0 as expected, and in the large α limit we recover the Gauss-Bonnet model with potential and coupling function of the form φ 2n . We study perturbations and non-Gaussianity in this setup and we find some constraints on the model's parameters in comparison with PLANCK data sets. We study also the reheating epoch after inflation in this setup. For this purpose, we seek the number of e-folds and temperature during reheating epoch. These quantities depend on the model's parameter and the effective equation of state of the dominating energy density in the reheating era. We find some observational constraints on these parameters.PACS numbers: 04.50. Kd , 98.80.Cq , 98.80.Es

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Further Refining Swampland Conjecture on Inflation in General Scalar‐Tensor Theories of Gravity

Yuennan

Channuie

2022

Fortschritte der Physik

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An alternative refined de Sitter conjecture giving rise to a natural combination of the first and second derivatives of the scalar potential was proposed recently by David Andriot and Christoph Roupec (Fortsch. Phys. 67 (2019) no.1‐2, 1800105). In this work, we study the inflation models in a general scalar‐tensor theory with exponential and hyperbolic tangent forms of potential as well as model with quantum corrected potential and examine whether these three models of inflation can satisfy this further refining de Sitter swampland conjecture or not. Regarding our analysis with proper choices of parameters a,b=1−a$a, b=1- a$ and q, we find that these three inflationary models can always satisfy this new refined swampland conjecture. Therefore, all three inflationary models might all be in “landscape” since the “further refining de Sitter swampland conjecture” is satisfied.

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Constraints onα-attractor inflation and reheating

Cited by 104 publications

References 44 publications

Fiber inflation and reheating

Fiber inflation and reheating

Perturbation, non-Gaussianity, and reheating in a Gauss-Bonnet α -attractor model

Further Refining Swampland Conjecture on Inflation in General Scalar‐Tensor Theories of Gravity

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