Realistic equations of state for the primeval universe

Aldrovandi, R.; Cuzinatto, R. R.; Medeiros, L. G.

doi:10.1140/epjc/s10052-008-0780-6

Cited by 10 publications

(8 citation statements)

References 74 publications

(108 reference statements)

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“…Firstly we note in both figures that ω starts with negative values, specifically, when t ∼ 0, ω ∼ −1, independently of the model. This is in agreement with some constraints that were recently put to the inflationary EoS [55][56][57]. Note that this behavior is reflected in the curves of H(t) for small values of time (t → 0 ⇒ H(t) → constant).…”

Section: Discussionsupporting

confidence: 91%

Cosmological scenarios from multiquintessence

et al. 2018

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In this work we derive and analyse cosmological scenarios coming from multi-component scalar field models. We consider a direct sum of a sine-Gordon with a Z2 model, and also a combination of those with a BNRT model. Moreover, we work with a modified version of the BNRT model, which breaks the Z2 x Z2 symmetry of the original BNRT potential, coupled with the sine-Gordon and with the standard Z2 models. We show that our approach can be straightforwardly elevated to N fields. All the computations are made analytically and some parameters restriction is put forward in order to get in touch with complete and realistic cosmological scenarios.

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Section: Discussionsupporting

confidence: 91%

Cosmological scenarios from multiquintessence

et al. 2018

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“…By analysing it, one can see that for small values of time, ω ∼ −1. This is in agreement with some constraints that have been put to inflationary EoS recently [40]- [42].…”

Section: Cosmological Interpretationssupporting

confidence: 93%

A complete cosmological scenario from $f(R,T^φ)$ gravity theory

Moraes,

Santos

2016

Preprint

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Recent elaborated by T. Harko and collaborators, the f (R, T ) theories of gravity contemplate an optimistic alternative to dark energy, for which R and T stand for the Ricci scalar and the trace of the energymomentum tensor, respectively. Although the literature has shown that the T dependence on the gravitational part of the action -which is due to the consideration of quantum effects -may induce some novel features in the scope of late-time cosmological dynamics, in the radiation-dominated universe, when T = 0, no contributions seem to rise from such theories. Apparently, f (R, T ) contributions to a radiation-dominated universe may rise only from the f (R, T φ ) approach, which is nothing but the f (R, T ) gravity in the case of a self-interacting scalar field whose trace of the energymomentum tensor is T φ . We intend, in this article, to show how f (R, T φ ) theories of gravity can contribute to the study of the primordial stages of the universe. Our results predict a graceful exit from inflationary stage to a radiation-dominated era. They also predict a late-time cosmic acceleration after a matter-dominated phase, making the f (R, T φ ) theories able to describe, in a self-consistent way, all the different stages of the universe dynamics.

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“…By analyzing it, one can see that for small values of time, ω ∼ −1. This is in agreement with some constraints that have been put to inflationary EoS recently [40][41][42].…”

Section: Cosmological Interpretationssupporting

confidence: 93%

A complete cosmological scenario from $$f(R,T^{\phi })$$ f ( R , T ϕ )

Moraes¹,

Santos²

2016

Eur. Phys. J. C

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Recent elaborated by Harko et al., the f (R, T ) theories of gravity allow one to contemplate an optimistic alternative to dark energy, for which R and T stand for the Ricci scalar and the trace of the energy-momentum tensor, respectively. Although the literature has shown that the T dependence on the gravitational part of the action -which is due to the consideration of quantum effects -may induce some novel features in the scope of late-time cosmological dynamics, in the radiation-dominated universe, when T = 0, no contributions seem to arise from such theories. Apparently, f (R, T ) contributions to a radiation-dominated universe may arise only from the f (R, T φ ) approach, which is nothing but the f (R, T ) gravity in the case of a selfinteracting scalar field whose trace of the energy-momentum tensor is T φ . We intend, in this article, to show how f (R, T φ ) theories of gravity can contribute to the study of the primordial stages of the universe. Our results predict a graceful exit from an inflationary stage to a radiation-dominated era. They also predict a late-time cosmic acceleration after a matter-dominated phase, enabling the f (R, T φ ) theories to describe, in a self-consistent way, all the different stages of the dynamics of the universe.

show abstract

Realistic equations of state for the primeval universe

Cited by 10 publications

References 74 publications

Cosmological scenarios from multiquintessence

Cosmological scenarios from multiquintessence

A complete cosmological scenario from $f(R,T^φ)$ gravity theory

A complete cosmological scenario from $$f(R,T^{\phi })$$ f ( R , T ϕ )

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