Growth rate in the dynamical dark energy models

Avsajanishvili, Olga; Arkhipova, N. A.; Samushia, Lado; Kahniashvili, Tina

doi:10.1140/epjc/s10052-014-3127-5

Cited by 24 publications

(24 citation statements)

References 54 publications

(51 reference statements)

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“…Recent studies have considered the PR-potential in the light of the cosmological data, see e.g. [30,31,32,33,34]. Here we show that the asset of current observations indicates strong signs of dynamical DE which can be parametrized with such potential.…”

Section: φCdm With Peebles and Ratra Potentialsupporting

confidence: 66%

Dynamical dark energy: Scalar fields and running vacuum

2017

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Recent analyses in the literature suggest that the concordance ΛCDM model with rigid cosmological term, Λ =const., may not be the best description of the cosmic acceleration. The class of "running vacuum models", in which Λ = Λ(H) evolves with the Hubble rate, has been shown to fit the string of SNIa+BAO+H(z)+LSS+CMB data significantly better than the ΛCDM. Here we provide further evidence on the time-evolving nature of the dark energy (DE) by fitting the same cosmological data in terms of scalar fields. As a representative model we use the original Peebles & Ratra potential, V ∝ φ −α . We find clear signs of dynamical DE at ∼ 4σ c.l., thus reconfirming through a nontrivial scalar field approach the strong hints formerly found with other models and parametrizations.

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Section: φCdm With Peebles and Ratra Potentialsupporting

confidence: 66%

Dynamical dark energy: Scalar fields and running vacuum

2017

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“…When α=0 the fCDM model is reduced to the corresponding ΛCDM scenario. The fCDM model with this kind of V(f) has been extensively investigated, mostly in the spatially flat case (Podariu & Ratra 2000;Chae et al 2004;Samushia et al 2007;Samushia & Ratra 2010;Chen & Ratra 2011a, 2011bFarooq & Ratra 2013;Farooq et al 2013aFarooq et al , 2013bAvsajanishvili et al 2014;Pavlov et al 2014;Chen et al 2015;Lima et al 2015), and only limited attention has been paid to the non-flat scenario (Pavlov et al 2013;Farooq et al 2015;Gosenca & Coles 2015). However, the above-mentioned literature on the fCDM model did not consider massive neutrinos.…”

Section: Introductionmentioning

confidence: 99%

Constraints on Non-Flat Cosmologies With Massive Neutrinos After Planck 2015

Chen

Ratra

Biesiada

et al. 2016

ApJ

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We investigate two dark energy cosmological models (i.e., the ΛCDM and fCDM models) with massive neutrinos assuming two different neutrino mass hierarchies in both the spatially flat and non-flat scenarios, where in the fCDM model the scalar field possesses an inverse power-law potential, V(f)∝f − α (α>0). Cosmic microwave background data from Planck2015, baryon acoustic oscillation data from 6dFGS, SDSS-MGS, BOSS-LOWZ and BOSS CMASS-DR11, the joint light-curve analysis compilation of SNe Ia apparent magnitude observations, and the Hubble Space Telescope H 0 prior, are jointly employed to constrain the model parameters. We first determine constraints assuming three species of degenerate massive neutrinos. In the spatially flat (non-flat) ΛCDM model, the sum of neutrino masses is bounded as Σm ν <0.165(0.299) eV at 95% confidence level (CL). Correspondingly, in the flat (non-flat) fCDM model, we find Σm ν <0.164(0.301) eV at 95% CL. The inclusion of spatial curvature as a free parameter results in a significant broadening of confidence regions for Σm ν and other parameters. In the scenario where the total neutrino mass is dominated by the heaviest neutrino mass eigenstate, we obtain similar conclusions to those obtained in the degenerate neutrino mass scenario. In addition, the results show that the bounds on Σm ν based on two different neutrino mass hierarchies have insignificant differences in the spatially flat case for both the ΛCDM and fCDM models; however, the corresponding differences are larger in the nonflat case.

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“…Although one parameter (∆) formula is investigated in the reference [16] and some interesting features are predicted, our work introduces two more parameters and various other possibilities are predicted under the observational constraint [20]. There are many other trials to investigate w(z) of dark energy and they have the original perspective in the quintessence scenario [10][11][12][13][14][15][16][17][18][19][20][21][22][23]. We believe that it is urgent to determine ∆ > 0 for quintessence and other models.…”

Section: Resultsmentioning

confidence: 99%

“…We have taken the exact approach [11,12] to investigate five different exact potentials, not taken the approximate parametrization approach for w [13,14]. We have also mainly concerned the terminal boundary condition at z ≃ 0 [11][12][13][14][15][16][17][18][19][21][22][23] and not z ≫ 1 [4,11,15,17]. Adding to the above-mentioned points, there are two more new aspects of this paper, 1) We have imposed a new constraint on w(z), which was discovered in Ref.…”

Section: Introductionmentioning

confidence: 99%

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Constraints for the thawing and freezing potentials

Hara

Suzuki

Saka

et al. 2018

Progress of Theoretical and Experimental Physics

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We study the accelerating present universe in terms of the time evolution of the equation of state w(z) (redshift z) due to thawing and freezing scalar potentials in the quintessence model.The values of dw/da and d 2 w/da 2 at scale factor of a = 1 are associated with two parameters of each potential. For five type scalar potentials, the scalar fields Q and w as function of time t and/or z are numerically calculated under the fixed boundary condition of w(z = 0) = −1 + ∆.The observational constraint w obs (Planck 2015) is imposed to test whether the numerical w(z) is in w obs . Some solutions show the thawing features in the freezing potentials. Mutually exclusive allowed regions in dw/da vs. d 2 w/da 2 diagram are obtained in order to identify the likely scalar potential and even the potential parameters by future observational tests.

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Growth rate in the dynamical dark energy models

Cited by 24 publications

References 54 publications

Dynamical dark energy: Scalar fields and running vacuum

Dynamical dark energy: Scalar fields and running vacuum

Constraints on Non-Flat Cosmologies With Massive Neutrinos After Planck 2015

Constraints for the thawing and freezing potentials

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