An interacting new holographic dark energy model: Observational constraints

Sadri, Ehsan; Khurshudyan, Martiros

doi:10.1142/s0218271819501529

Cited by 19 publications

(11 citation statements)

References 91 publications

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“…Finally, it is important to mention that holographic models for dark energy are supported by the observational data and exhibit a consistent matter growth perturbations and stability [7,23,32,43].…”

Section: Final Remarksmentioning

confidence: 60%

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Modeling holographic dark energy with particle and future horizons

Cruz

Lepe

2020

Nuclear Physics B

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In this work we explore some properties and their implications at thermodynamics level of the particle and future horizons when are considered as candidates to model the dark energy within a holographic context for a flat Friedmann-Lemaitre-Robertson-Walker universe. Under these considerations we can find that the model admits a genuine big rip singularity when the dark energy density is sketched by the future horizon, in consequence the resulting parameter state can cross to the phantom regime. For the particle horizon case the cosmological fluid can emulate ordinary matter. Additionally, the coincidence parameter has a decreasing behavior for the future horizon. On the other hand, from the interacting scheme for cosmological fluids we obtain that in the dark energy -dark matter interaction, the dark energy fluid will have negative entropy production, therefore the second law of thermodynamics can not be guaranteed in this sector. PACS numbers: 95.36.+x, 95.35.+d,

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Section: Final Remarksmentioning

confidence: 60%

“…See also Ref. [43], where was found that the interacting scheme for holographic dark energy evolves in agreement with observational data and exhibits stability, and Ref. [44], where the inclusion of spatial curvature in the interacting scheme leads to an expanding and accelerating universe.…”

Section: B Interacting Cosmological Fluidsmentioning

confidence: 63%

Modeling holographic dark energy with particle and future horizons

Cruz

Lepe

2020

Nuclear Physics B

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“…The interaction term proportional to the DE density or to the DM density or to a linear combination of both densities was well studied in literature [52,53,54,55]. But in some literature [39,40,56,57,37,58] the non linear interaction i.e., an interaction proportional to the product of DM density and DE energy density were studied and found to be favored observationally than linear interaction between dark sectors [41]. The general form for the nonlinear interaction can be written as [39],…”

Section: The Model : Holographic Ricci De As Running Vacuum With Nonl...mentioning

confidence: 99%

Holographic Ricci DE as running vacuum with nonlinear interactions

George¹

2022

Preprint

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The holographic Ricci dark energy can be treated as a running vacuum due to its analogy in the energy density, which is a combination of H and Ḣ, the model can predict either eternal acceleration or eternal deceleration. In the earlier works, we have shown that the presence of additive constant in the energy density or by considering possible interaction between dark sectors through a phenomenological term, the model can predict a transition from a prior decelerated to a late accelerated epoch. This paper analyses the cosmic evolution of holographic Ricci dark energy as running vacuum with a nonlinear interaction between dark sectors in a flat FLRW universe. We consider three possible nonlinear interaction forms which give analytically feasible solutions. We have constrained the model using the Type1a Supernova(Pantheon)+CMB(Planck 2018)+BAO(SDSS) data and evaluated the best-estimated values of all the model parameters. We have analyzed the evolution of the Hubble parameter and deceleration parameter of all three cases. We perform state finder analysis of the model, which implies the quintessence nature of the model and found that it is distinguishably different from the standard ΛCDM model. The dynamical system analysis of all three cases confirms the evolution of the universe from an unstable prior matter-dominated era to a stable end de Sitter phase.

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“…Interacting holographic dark energy models are discussed in Ref. [20]. Models of future singularities are classified in Ref.…”

Section: Introductionmentioning

confidence: 99%

Viscous coupled fluids in terms of a log-corrected equation of state

Brevik,

Myrzakulov,

Timoshkin

et al. 2021

Preprint

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We consider a class of cosmological fluids that possess properties analogous to those of crystalline solids undergoing isotropic deformations. Our research is based on a modified log-corrected powerlaw equation of state in the presence of a bulk viscosity. This formalism represents a class of so-called logotropic fluids, and allows explaining an accelerating late-time universe. In order to obtain a more detailed picture of its evolution, we add in our model a coupling of the log-corrected power-law fluid to dark matter, and study various interacting forms between them. We solve the system of equations for a modified log-power-law fluid coupled to dark matter, and obtain expressions for the log-corrected power-law energy density, and the energy density for dark matter.A comparative analysis is made with the model of a nonviscous log-corrected power-law fluid without interaction with dark matter.

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An interacting new holographic dark energy model: Observational constraints

Cited by 19 publications

References 91 publications

Modeling holographic dark energy with particle and future horizons

Modeling holographic dark energy with particle and future horizons

Holographic Ricci DE as running vacuum with nonlinear interactions

Viscous coupled fluids in terms of a log-corrected equation of state

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