A polynomial f(R) inflation model

Huang, Qing-Guo

doi:10.1088/1475-7516/2014/02/035

Cited by 129 publications

(91 citation statements)

References 40 publications

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“…Such a formalism successfully describes both the inflationary era [7,8] and the current phase of accelerated expansion our Universe is undergoing [9,10], the latter, with no need of a CC.…”

Section: Introductionmentioning

confidence: 99%

Information content inF(R)brane models with nonconstant curvature

et al. 2015

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In this work we investigate the entropic information-measure in the context of braneworlds with non-constant curvature. The braneworld entropic information is studied for gravity modified by the squared of the Ricci scalar, besides the usual Einstein-Hilbert term. We showed that the minimum value of the brane configurational entropy provides a stricter bound on the parameter that is responsible for the F (R) model to differ from the Einstein-Hilbert standard one. Our results are moreover consistent to a negative bulk cosmological constant.

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“…Such a formalism successfully describes both the inflationary era [7,8] and the current phase of accelerated expansion our Universe is undergoing [9,10], the latter, with no need of a CC.…”

Section: Introductionmentioning

confidence: 99%

Information content inF(R)brane models with nonconstant curvature

et al. 2015

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“…In the present paper we study the simplest f (R) theory, namely R + βR N . This theory has been well-investigated in the Einstein frame in the context of inflationary dynamics ( [43][44][45]). The scalaron potential in the chosen unit system (footnote 2) has the following form,…”

Section: The Model and A Picture In The Einstein Framementioning

confidence: 99%

“…Finally from (43,44,45) the Hubble parameter and the matter energy density as functions of time are given by…”

Section: First Order Solution Of the Perturbed Systemmentioning

confidence: 99%

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Asymptotic solutions in f(R)-gravity

Bukzhalev

Ivanov

Toporensky

2014

Class. Quantum Grav.

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We study cosmological solutions in R + βR N -gravity for an isotropic Universe filled with ordinary matter with the equation of state parameter γ. Using the BogolyubovKrylov-Mitropol'skii averaging method we find asymptotic oscillatory solutions in terms of new functions, which have been specially introduced by us for this problem and appeared as a natural generalization of the usual sine and cosine. It is shown that the late-time behaviour of the Universe in the model under investigation is determined by the sign of the difference γ − γ crit where γ crit = 2N/(3N − 2). If γ < γ crit , the Universe reaches the regime of small oscillations near values of Hubble parameter and matter density, corresponding to General Relativity solution. Otherwise higher-curvature corrections become important at late times. We also study numerically basins of attraction for the oscillatory and phantom solutions, which are present in the theory for N > 2. Some important differences between N = 2 and N > 2 cases are discussed. *

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“…It was demonstrated that the slow-roll inflation can be achieved as long as the dimensionless coupling λ n is sufficiently small [11].…”

Section: Introductionmentioning

confidence: 99%

Starobinsky cosmological model in Palatini formalism

Stachowski

Szydłowski

Borowiec³

2017

Eur. Phys. J. C

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We classify singularities in FRW cosmologies, which dynamics can be reduced to the dynamical system of the Newtonian type. This classification is performed in terms of the geometry of a potential function if it has poles. At the sewn singularity, which is of a finite scale factor type, the singularity in the past meets the singularity in the future. We show that such singularities appear in the Starobinsky model in f (R) =R + γR 2 in the Palatini formalism, when dynamics is determined by the corresponding piecewise-smooth dynamical system. As an effect we obtain a degenerate singularity. Analytical calculations are given for the cosmological model with matter and the cosmological constant. The dynamics of model is also studied using dynamical system methods. From the phase portraits we find generic evolutionary scenarios of the evolution of the universe. For this model, the best fit value of γ = 3γ H 2 0 is equal 9.70 × 10 −11 . We consider a model in both Jordan and Einstein frames. We show that after transition to the Einstein frame we obtain both the form of the potential of the scalar field and the decaying Lambda term.

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A polynomial f(R) inflation model

Cited by 129 publications

References 40 publications

Information content inF(R)brane models with nonconstant curvature

Information content inF(R)brane models with nonconstant curvature

Asymptotic solutions in f(R)-gravity

Starobinsky cosmological model in Palatini formalism

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