Non-local scalar fields inflationary mechanism in light of Planck 2013

Sheikhahmadi, Haidar; Ghorbani, Soheyla; Saaidi, Kh.

doi:10.1007/s10509-015-2343-2

Cited by 10 publications

(6 citation statements)

References 67 publications

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“…A general classification of inflationary models is divided as cold and warm inflation. In cold inflation [10][11][12][13][14], where the scalar field is dominant component and its interaction with other fields could be ignored, quantum perturbations are the source for cosmic microwaves background anisotropy and large scale structure as well. However, in warm inflation [15][16][17][18][19][20][21], scalar field, that is still the dominant component, interacts with other fields and decays through expansion into radiation and other fields [19,20].…”

Section: Introductionmentioning

confidence: 99%

Viscous warm inflation: Hamilton–Jacobi formalism

Akhtari

Mohammadi

Sayar

et al. 2017

Astroparticle Physics

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Using Hamilton-Jacobi formalism, the scenario of warm inflation with viscous pressure is considered. The formalism gives a way of computing the slow-rolling parameter without extra approximation, and it is well-known as a powerful method in cold inflation. The model is studied in detail for three different cases of the dissipation and bulk viscous pressure coefficients. In the first case where both coefficients are taken as constant, it is shown that the case could not portray warm inflationary scenario compatible with observational data even it is possible to restrict the model parameters. For other cases, the results shows that the model could properly predicts the perturbation parameters in which they stay in perfect agreement with Planck data. As a further argument, r − n s and α s − n s are drown that show the acquired result could stand in acceptable area expressing a compatibility with observational data.

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Section: Introductionmentioning

confidence: 99%

Viscous warm inflation: Hamilton–Jacobi formalism

Akhtari

Mohammadi

Sayar

et al. 2017

Astroparticle Physics

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“…Even better, inflation theory provides a mechanism to explain structure formation and the source of the observed anisotropies in the Cosmic Microwave Background (CMB) radiation (Larson 2011;Bennett et al 2011;Jarosik 2011). Besides, this scenario can estimate a correct result for the amplitude of primordial perturbations compared to observations ( Bassett et al 2006;Liddle 1999;Langlois 2004;Lyth 1997;Lyth & Riotto 1999;Guth 2000;Lidsey et al 1997;Mukhanov et al 1992;Sheikhahmadi et al 2015;Sheikhahmadi et al 2016;Sheikhahmadi 2018). Many various inflationary models have been investigated in (Brandenberger 1999;Liddle & Lyth 2000), that could be divided into two parts well-known as super cold and warm inflationary proposals.…”

Section: Introductionmentioning

confidence: 57%

Constraints on warm power-law inflation in light of Planck results

Ghadiri¹,

Refaei²,

Aghamohammadi³

et al. 2018

Preprint

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The constraints on a general form for powerlaw potential in the framework of warm single field inflation by means of Planck 2013 and 2015 will be investigated. By considering much less dynamic universe, quasi-static evolutions, and also the well-known slowroll conditions the regions which a binary of our free parameters are in good agreement with Planck results will be obtained. The advantage of this likelihood method is that instead of a set of free parameters we can visualize a region of free parameters that can satisfy the precision limits on theoretical results. On the other side, when we consider the preformed quantity for the amplitude of scalar perturbations the conflict between obtained results for free parameters in different steps dramatically decreased. As done in flagship literature, based on the friction of the environment, we can divide the primordial universe into two different epochs namely weak and strong dissipative regimes. For the aforementioned eras, the free parameters of the model will be constrained and the best regions will be obtained. To do so the main inflationary observables such as tensor-to-scalar ratio, power-spectra of density perturbations and gravitational waves, scalar and tensor

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“…Following [16], and from the observational point of view, we can classify the huge number of different models of inflation into three main categories, with their related sub-categories. These are the single-field inflation [61][62][63][64][65][66][67][68][69][70][71][72][73][74], the multiple-field inflation [75][76][77][78][79][80][81][82] and those models in which the fluid is not described by scalar fields [83][84][85][86][87].…”

Section: Introductionmentioning

confidence: 99%

Constraining chameleon field driven warm inflation with Planck 2018 data

et al. 2019

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We investigate warm inflationary scenario in which the accelerated expansion of the early Universe is driven by chameleon-like scalar fields. Due to the non-minimal coupling between the scalar field and the matter sector, the energy-momentum tensor of each fluid component is not conserved anymore, and the generalized balance equation is obtained. The new source term in the energy equation can be used to model warm inflation. On the other hand, if the coupling function varies slowly, the model reduces to the standard model used for the description of cold inflation. To test the validity of the warm chameleon inflation model, the results for warm inflationary scenarios are compared with the observational Planck2018 Cosmic Microwave Background data. In this regard, the perturbation parameters such as the amplitude of scalar perturbations, the scalar spectral index and the tensor-to-scalar ratio are derived at the horizon crossing in two approximations, corresponding to the weak and strong dissipative regimes. As a general result it turns out that the theoretical predictions of the chameleon warm inflationary scenario are consistent with the Planck 2018 observations.

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Non-local scalar fields inflationary mechanism in light of Planck 2013

Cited by 10 publications

References 67 publications

Viscous warm inflation: Hamilton–Jacobi formalism

Viscous warm inflation: Hamilton–Jacobi formalism

Constraints on warm power-law inflation in light of Planck results

Constraining chameleon field driven warm inflation with Planck 2018 data

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