On the holographic dark energy in chameleon scalar-tensor cosmology

A generalization of the canonical and non-canonical theory of inflation is introduced in which the kinetic energy term in action is written as non-local term. The inflationary universe within the framework of considering this non-locality will be studied. To investigate the effects of non-locality on the inflationary parameters we consider two well known models of inflationary scenario includes of chaotic and exponential inflation proposals. For such scenarios some important parameters include slow roll parameters, scalar and tensor power spectra, spectral indices, the tensor-to-scalar ratio and so on for both mentioned models, chaotic and exponential inflationary scenarios, will be calculated. Also the Hamilton-Jacobi formalism, as an easiest way to study the effect of perturbation based on e-folding number N , to investigate inflationary attractors will be used. The free theoretical parameters of this model will be compared with observations by means of Planck 2013, W M AP 9 + eCM B + BAO + H 0 data sets in addition to BICEP 2 data surveying. It will be shown that our theoretical results are in acceptable range in comparison to observations. For instance the tensor-to-scalar ratio for exponential potential, by considering BICEP 2 is in best agreement in comparison with chaotic inflation.

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“…Using definition of n s and this fact that d d ln k = − d dN , combination of Eqs. (40) and (42) yields…”

Section: Chaotic Inflationmentioning

confidence: 98%

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

Sheikhahmadi

Ghorbani

Saaidi

2015

Astrophys Space Sci

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“…There are many studies on this topic such as [184][185][186][187][188][189][190][191][192], where the authors explain that there are two definitions for the Lagrangian of a perfect fluid as L (2) m = p, respectively. However, in our case, this degeneracy is broken due to the non-minimal interaction of the scalar field and matter, and therefore we follow the approach proposed in [192], where it is shown that only for L (2) m = p one has a geodesic motion for perfect fluids.…”

Section: )mentioning

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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“…Also, much attempts have been done to reconstruct scalar field DE models, from HDE and ADE [42][43][44][45][46]. In some of them the coupling between the scalar field and DM Lagrangian, called chameleon, has been considered [47][48][49]. Tachyon scalar field motivated from string theory is a especial scalar field which can explain the whole history of the Universe from inflation to late time acceleration [50][51][52][53][54][55][56][57][58][59].…”

Section: Issn: 2641-886xmentioning

confidence: 99%

Interacting Logarithmic Entropy-Corrected Agegraphic Chameleon-Tachyon Dark Energy

Ravanpak¹,

Fadakar²

2019

Int J Cosmol Astron Astrophys

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Considering entropy correction terms resulting from loop quantum gravity, we investigate an interacting agegraphic dark energy model. The connection between such a model and a tachyon scalar field which couples to matter in Lagrangian is studied. We reconstruct the related potential of tachyon field and find its dynamics in the Universe. Also, we discuss the implications of this entropy-corrected agegraphic dark energy model.

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On the holographic dark energy in chameleon scalar-tensor cosmology

Cited by 10 publications

References 87 publications

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

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

Constraining chameleon field driven warm inflation with Planck 2018 data

Interacting Logarithmic Entropy-Corrected Agegraphic Chameleon-Tachyon Dark Energy

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