Model of interacting holographic dark energy at the Ricci scale

Durán, I.; Pavón, Diego

doi:10.1103/physrevd.83.023504

Cited by 61 publications

(56 citation statements)

References 54 publications

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“…In particular, we obtain ρ x ∝ R for α = 4/3 [13], where R = 6(Ḣ + 2H 2 ) is the Ricci scalar curvature for a spatially flat FRW spacetime.…”

Section: The Modelmentioning

confidence: 99%

“…Using the largest L as the one saturating the above inequality, it turns out to be the holographic dark energy is given by ρ x = 3c 2 M 2 P L −2 , where c is a numerical factor. The IR cutoff has been taken as the large scale of the universe, Hubble horizon [6,7], particle horizon, event horizon [7] or generalized IR cutoff [8], [9], [10], [11] [12], [13], [14], [15] amongst many others. One of the main reasons in working within the framework of dynamical dark energy such as a HDE relies on the need of explaining the current accelerated a Electronic address: chimento@df.uba.ar b Electronic address: monicaforte@fibertel.com.ar c Electronic address: martin@df.uba.ar phase of the Universe; this fact has been confirmed by a plethora of observational tests such as high redshift Hubble diagram of type Ia supernovae as standard candles [16][17][18][19] and accurate measurements of cosmic microwave background (CMB) anisotropies [20][21][22].…”

Section: Introductionmentioning

confidence: 99%

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Modified holographic Ricci dark energy coupled to interacting dark matter and a non-interacting baryonic component

2013

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We examine a Friedmann-Robertson-Walker universe filled with interacting dark matter, modified holographic Ricci dark energy (MHRDE), and a decoupled baryonic component.The estimations of the cosmic parameters with Hubble data lead to an age of the universe of 13.17 Gyr and show that the MHRDE is free from the cosmic-age problem at low redshift (0 ≤ z ≤ 2) in contrast to holographic Ricci dark energy (HRDE) case. We constrain the parameters with the Union2 data set and contrast with the Hubble data. We also study the behavior of dark energy at early times by taking into account the severe bounds found at recombination era and/or at big bang nucleosynthesis. The inclusion of a non interacting baryonic matter forces that the amount of dark energy at zt ∼ O(1) changes abruptly implying that Ωx(z ≃ 1100) = 0.03, so the bounds reported by the forecast of Planck and CMBPol experiments are more favored for the MHRDE model than in the case of HRDE cutoff. For the former model, we also obtain that at high redshift the fraction of dark energy varies from 0.006 to 0.002, then the amount of Ωx at the big bang nucleosynthesis era does not disturb the observed Helium abundance in the universe provided that the bound Ωx(z ≃ 10 10 ) < 0.21 is hold.

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“…In particular, we obtain ρ x ∝ R for α = 4/3 [13], where R = 6(Ḣ + 2H 2 ) is the Ricci scalar curvature for a spatially flat FRW spacetime.…”

Section: The Modelmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Modified holographic Ricci dark energy coupled to interacting dark matter and a non-interacting baryonic component

2013

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“…To obtain new scientific results, new elements need to be taken into account. Since the interaction between different components widely exist in nature, and the introduction of a interaction between DE and CDM can provide an intriguing mechanism to solve the "cosmic coincidence problem" (Guo et al 2007;Li et al 2009b,a;He et al 2010) and alleviate the "cosmic age problem" Wang et al 2010;Cui & Zhang 2010;Durán & Pavón 2011), it is interesting to study the effect of different LCF on interacting dark energy (IDE) model. Here we adopt the w-cold-dark-matter (wCDM) model with a direct non-gravitational interaction between dark sectors.…”

Section: Introductionmentioning

confidence: 99%

Impacts of different SNLS3 light-curve fitters on cosmological consequences of interacting dark energy models

et al. 2016

A&A

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We explore the cosmological consequences of interacting dark energy (IDE) models using the SNLS3 supernova samples. In particular, we focus on the impacts of different SNLS3 light-curve fitters (LCF; referred to in this paper as SALT2, SiFTO and combined sample). Firstly, making use of the three SNLS3 data sets, as well as the Planck distance priors data and the galaxy clustering data, we constrain the parameter spaces of three IDE models. Then, we study the cosmic evolutions of Hubble parameter H(z), deceleration diagram q(z), statefinder hierarchy S 4 (z), and check whether or not these dark energy diagnosis can distinguish the differences among the results of different SNLS3 LCF. Finally, we perform a high redshift cosmic age test using three old high redshift objects (OHRO), and explore the fate of the Universe. We find that the impacts of different SNLS3 LCF are rather small, and can not be distinguished using H(z), q(z), S 4 (z), and the age data of OHRO. In addition, we infer, from the current observations, how far we are from a cosmic doomsday in the worst case, and find that the combined sample always gives the largest 2σ lower limit of the time interval between "big rip" and today, while the results given by the SALT2 and the SiFTO sample are similar. These conclusions are insensitive to a specific form of dark sector interaction. Our method can be used to distinguish the differences among various cosmological observations.

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“…a non gravitational interaction between DE and dark matter (DM)) at Ricci scale, in which L = (Ḣ + 2H 2 ) −1/2 has been proposed. The authors performed a detailed discussion on the cosmic coincidence problem, age problem and obtained some observational constraints on their's model [15].…”

Section: Introductionmentioning

confidence: 99%

Interacting entropy-corrected holographic dark energy with apparent horizon as an infrared cutoff

Khodam-Mohammadi

Malekjani

2012

Gen Relativ Gravit

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In this work we consider the entropy-corrected version of interacting holographic dark energy (HDE), in the non-flat universe enclosed by apparent horizon. Two corrections of entropy so-called logarithmic 'LEC' and power-law 'PLEC' in HDE model with apparent horizon as an IR-cutoff are studied. The ratio of dark matter to dark energy densities u, equation of state parameter w D and deceleration parameter q are obtained. We show that the cosmic coincidence is satisfied for both interacting models. By studying the effect of interaction in EoS parameter, we see that the phantom divide may be crossed and also find that the interacting models can drive an acceleration expansion at the present and future, while in non-interacting case, this expansion can happen only at the early time. The graphs of deceleration parameter for interacting models, show that the present acceleration expansion is preceded by a sufficiently long period deceleration at past.Moreover, the thermodynamical interpretation of interaction between LECHDE and dark matter is described. We obtain a relation between the interaction term of dark components and thermal fluctuation in a non-flat universe, bounded by the apparent horizon. In limiting case, for ordinary HDE, the relation of interaction term versus thermal fluctuation is also calculated. *

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Model of interacting holographic dark energy at the Ricci scale

Cited by 61 publications

References 54 publications

Modified holographic Ricci dark energy coupled to interacting dark matter and a non-interacting baryonic component

Modified holographic Ricci dark energy coupled to interacting dark matter and a non-interacting baryonic component

Impacts of different SNLS3 light-curve fitters on cosmological consequences of interacting dark energy models

Interacting entropy-corrected holographic dark energy with apparent horizon as an infrared cutoff

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