Scalar Field Cosmology

Chervon, S. V.; Фомин, И. В.; Yurov, V. A.; Yurov, Artyom V.

doi:10.1142/11405

Cited by 39 publications

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“…with the same relation (97) between scalar fields φ GB and φ E . Thus, expressions (93)-(98) or (106)-(114) completely determine the relations between exact inflationary solutions in the case of Einstein gravity (see, for example, in [10,12,75,76]) and approximate ones for a weak GB coupling. The difference between the solutions is determined by a coupling constant α GB .…”

Section: Background Dynamic Equations In Terms Of a Scalar Fieldmentioning

confidence: 99%

“…(106)-(107) by the choice of the Hubble parameter H E = H E (φ E ) as the function of a scalar field φ E . 2 A review of this method is given in [10,12].…”

Section: Background Dynamic Equations In Terms Of a Scalar Fieldmentioning

confidence: 99%

“…Thus, background dynamic Eqs. (111)-(112) can be considered as the Hamilton-Jacobi type equations [74] or, otherwise, the Ivanov-Salopek-Bond equations [10,12] by analogy with the case of GR, for a special class of EGB inflationary models with the deviation parameter (90).…”

Section: Background Dynamic Equations In Terms Of a Scalar Fieldmentioning

confidence: 99%

“…At the moment, a many models of cosmological inflation with different scalar field potentials and different specifics of its evolution are considered to describe the evolution of the universe. A large number of inflationary models of the early universe based on Einstein gravity was considered in [9][10][11][12].…”

Section: The Examples Of Inflationary Models With a Weak Gb Couplingmentioning

confidence: 99%

“…Also, according to the theory of cosmological perturbations, quantum fluctuations of a scalar field induce corresponding perturbations of the metric, which give rise to a large-scale structure of the universe and relic gravitational waves [8]. At the moment, a large number of different models of cosmological inflation with canonical scalar fields based on Einstein gravity are considered to describe the inflationary stage of the evolution of universe [9][10][11][12].…”

Section: Introductionmentioning

confidence: 99%

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Gauss–Bonnet term corrections in scalar field cosmology

Фомин

2020

Eur. Phys. J. C

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The influence of non-minimal coupling of a scalar field and the Gauss–Bonnet term on the inflationary stage of evolution of the universe is investigated in this paper. The main cosmological effects of such a coupling were considered. The deviations between Einstein–Gauss–Bonnet inflation and standard one based on Einstein gravity were determined. The corrections of a weak GB coupling preserving the type of the scalar field potential to standard inflationary models is considered as well.

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Section: Background Dynamic Equations In Terms Of a Scalar Fieldmentioning

confidence: 99%

“…(106)-(107) by the choice of the Hubble parameter H E = H E (φ E ) as the function of a scalar field φ E . 2 A review of this method is given in [10,12].…”

Section: Background Dynamic Equations In Terms Of a Scalar Fieldmentioning

confidence: 99%

Section: Background Dynamic Equations In Terms Of a Scalar Fieldmentioning

confidence: 99%

Section: The Examples Of Inflationary Models With a Weak Gb Couplingmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Gauss–Bonnet term corrections in scalar field cosmology

Фомин

2020

Eur. Phys. J. C

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Canonical scalar field inflation with string and R2-corrections

2021

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Assuming that a scalar field controls the inflationary era, we examine the combined effects of string and f (R) gravity corrections on the inflationary dynamics of canonical scalar field inflation, imposing the constraint that the speed of the primordial gravitational waves is equal to that of light's. Particularly, we study the inflationary dynamics of an Einstein-Gauss-Bonnet gravity in the presence of αR 2 corrections, where α is a free coupling parameter. As it was the case in the pure Einstein-Gauss-Bonnet gravity, the realization that the gravitational waves propagate through spacetime with the velocity of light, imposes the constraint that the Gauss-Bonnet coupling function ξ(φ) obeys the differential equationξ = Hξ, where H is the Hubble rate. Subsequently, a relation for the time derivative of the scalar field is extracted which implies that the scalar functions of the model, which are the Gauss-Bonnet coupling and the scalar potential, are interconnected and simply designating one of them specifies the other immediately. In this framework, it is useful to freely designate ξ(φ) and extract the corresponding scalar potential from the equations of motion but the opposite is still feasible. We demonstrate that the model can produce a viable inflationary phenomenology and for a wide range of the free parameters. Also, a mentionable issue is that when the coupling parameter α of the R 2 correction term is α < 10 −3 in Planck Units, the R 2 term is practically negligible and one obtains the same equations of motion as in the pure Einstein-Gauss-Bonnet theory, however the dynamics still change, since now the time derivative of ∂f ∂R is nonzero. We study in detail the dynamics of inflation assuming that the slow-roll conditions hold true and also we briefly address the constant-roll case dynamics, and by using several illustrative examples, we compare the dynamics of the pure and R 2-corrected Einstein-Gauss-Bonnet gravity. Finally the ghosts issue is briefly addressed.

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Power-law f(R) gravity corrected canonical scalar field inflation

Oikonomou

2021

Annals of Physics

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Scalar Field Cosmology

Cited by 39 publications

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Gauss–Bonnet term corrections in scalar field cosmology

Gauss–Bonnet term corrections in scalar field cosmology

Canonical scalar field inflation with string and R2-corrections

Power-law f(R) gravity corrected canonical scalar field inflation

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