Identifying universality in warm inflation

Berera, Arjun; Mabillard, Joel; Pieroni, Mauro; Ramos, Rudnei O.

doi:10.1088/1475-7516/2018/07/021

Cited by 29 publications

(37 citation statements)

References 99 publications

(162 reference statements)

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“…We also note that the result (3.22) holds not only deep in the inflationary regime, but it also remains true through the end of inflation, when H → 1. This is because typically the ratio T /H increases towards the end of inflation, which is a common feature of the known models of WI [32,33].…”

Section: Jhep08(2020)127mentioning

confidence: 97%

Strengthening the de Sitter swampland conjecture in warm inflation

Brandenberger

Kamali

Ramos

2020

J. High Energ. Phys.

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The de Sitter constraint on the space of effective scalar field theories consistent with superstring theory provides a lower bound on the slope of the potential of a scalar field which dominates the evolution of the Universe, e.g., a hypothetical inflaton field. Whereas models of single scalar field inflation with a canonically normalized field do not obey this constraint, it has been claimed recently in the literature that models of warm inflation can be made compatible with it in the case of large dissipation. The de Sitter constraint is known to be derived from entropy considerations. Since warm inflation necessary involves entropy production, it becomes necessary to determine how this entropy production will affect the constraints imposed by the swampland conditions. Here, we generalize these entropy considerations to the case of warm inflation and show that the condition on the slope of the potential remains essentially unchanged and is, hence, robust even in the warm inflation dynamics. We are then able to conclude that models of warm inflation indeed can be made consistent with the swampland criteria.

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Section: Jhep08(2020)127mentioning

confidence: 97%

Strengthening the de Sitter swampland conjecture in warm inflation

Brandenberger

Kamali

Ramos

2020

J. High Energ. Phys.

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“…Then we will compare the predictions of the theoretical model with the Planck 2018 data. Following [85,87,103,119], the amplitude of the scalar perturbations is calculated to be…”

Section: Evolution Equations For Non-comoving Warm Inflationmentioning

confidence: 99%

Warm inflation with non-comoving scalar field and radiation fluid

Harkó

Sheikhahmadi

2021

Eur. Phys. J. C

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We consider a warm inflationary scenario in which the two major fluid components of the early Universe, the scalar field and the radiation fluid, evolve with distinct four-velocities. This cosmological configuration is equivalent to a single anisotropic fluid, expanding with a four-velocity that is a combination of the two fluid four-velocities. Due to the presence of anisotropies the overall cosmological evolution is also anisotropic. We obtain the gravitational field equations of the non-comoving scalar field–radiation mixture for a Bianchi Type I geometry. By assuming the decay of the scalar field, accompanied by a corresponding radiation generation, we formulate the basic equations of the warm inflationary model in the presence of two non-comoving components. By adopting the slow-roll approximation the theoretical predictions of the warm inflationary scenario with non-comoving scalar field and radiation fluid are compared in detail with the observational data obtained by the Planck satellite in both weak dissipation and strong dissipation limits, and constraints on the free parameters of the model are obtained. The functional forms of the scalar field potentials compatible with the non-comoving nature of warm inflation are also obtained.

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“…In the strong dissipative regime, the parameter G(Q), depending on the different values of the parameter m, can be approximated as [94,95]:…”

Section: Strong Dissipative Regimementioning

confidence: 99%

“…One of the important requirements of the inflationary scenarios is to establish a physically realistic relation between the end of the early accelerated, de Sitter type evolution, and the beginning of the radiation-dominated epoch, which corresponds to the SBB model. Based on this requirement, one can consider two different types of inflation, namely the super-cold and the warm models of inflation [88][89][90][91][92][93][94][95][96][97][98][99][100].…”

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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Identifying universality in warm inflation

Cited by 29 publications

References 99 publications

Strengthening the de Sitter swampland conjecture in warm inflation

Strengthening the de Sitter swampland conjecture in warm inflation

Warm inflation with non-comoving scalar field and radiation fluid

Constraining chameleon field driven warm inflation with Planck 2018 data

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