Thermodynamics second law and <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" altimg="si1.gif" overflow="scroll"><mml:mi>ω</mml:mi><mml:mo>=</mml:mo><mml:mo>−</mml:mo><mml:mn>1</mml:mn></mml:math> crossing(s) in interacting holographic dark energy model

Sadjadi, H. Mohseni; Honardoost, M.

doi:10.1016/j.physletb.2007.02.016

Cited by 68 publications

(10 citation statements)

References 56 publications

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“…Later on, it was argued that an interaction between the dark fluids, namely, DM and DE, can be used to provide a possible solution to the cosmic coincidence problem [556][557][558][559][560][561][562]. Additionally, an interaction in the dark sector can explain the phantom DE regime without any scalar field having a negative kinetic term [556,[563][564][565][566][567]. For those reasons, IDE scenarios have been substantially investigated in the literature, see e.g.…”

Section: Interacting Dark Energymentioning

confidence: 99%

In the realm of the Hubble tension—a review of solutions ^*

Valentino

Mena²,

Pan³

et al. 2021

Class. Quantum Grav.

1,302

760

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The simplest ΛCDM model provides a good fit to a large span of cosmological data but harbors large areas of phenomenology and ignorance. With the improvement of the number and the accuracy of observations, discrepancies among key cosmological parameters of the model have emerged. The most statistically significant tension is the 4σ to 6σ disagreement between predictions of the Hubble constant, H 0, made by the early time probes in concert with the ‘vanilla’ ΛCDM cosmological model, and a number of late time, model-independent determinations of H 0 from local measurements of distances and redshifts. The high precision and consistency of the data at both ends present strong challenges to the possible solution space and demands a hypothesis with enough rigor to explain multiple observations—whether these invoke new physics, unexpected large-scale structures or multiple, unrelated errors. A thorough review of the problem including a discussion of recent Hubble constant estimates and a summary of the proposed theoretical solutions is presented here. We include more than 1000 references, indicating that the interest in this area has grown considerably just during the last few years. We classify the many proposals to resolve the tension in these categories: early dark energy, late dark energy, dark energy models with 6 degrees of freedom and their extensions, models with extra relativistic degrees of freedom, models with extra interactions, unified cosmologies, modified gravity, inflationary models, modified recombination history, physics of the critical phenomena, and alternative proposals. Some are formally successful, improving the fit to the data in light of their additional degrees of freedom, restoring agreement within 1–2σ between Planck 2018, using the cosmic microwave background power spectra data, baryon acoustic oscillations, Pantheon SN data, and R20, the latest SH0ES Team Riess, et al (2021 Astrophys. J. 908 L6) measurement of the Hubble constant (H 0 = 73.2 ± 1.3 km s−1 Mpc−1 at 68% confidence level). However, there are many more unsuccessful models which leave the discrepancy well above the 3σ disagreement level. In many cases, reduced tension comes not simply from a change in the value of H 0 but also due to an increase in its uncertainty due to degeneracy with additional physics, complicating the picture and pointing to the need for additional probes. While no specific proposal makes a strong case for being highly likely or far better than all others, solutions involving early or dynamical dark energy, neutrino interactions, interacting cosmologies, primordial magnetic fields, and modified gravity provide the best options until a better alternative comes along.

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Section: Interacting Dark Energymentioning

confidence: 99%

In the realm of the Hubble tension—a review of solutions ^*

Valentino

Mena²,

Pan³

et al. 2021

Class. Quantum Grav.

1,302

760

View full text Add to dashboard Cite

show abstract

“…In [23], the authors have added the square of the Hubble parameter and its time derivative within the definition of holographic dark energy. While in [24], the authors propose a linear combination of particle horizon and the future event horizon. However, in this paper we stick to Li's proposal.…”

Section: Jcap03(2010)001mentioning

confidence: 99%

Interacting holographic dark energy with logarithmic correction

Jamil¹,

Farooq²

2010

J. Cosmol. Astropart. Phys.

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The holographic dark energy (HDE) is considered to be the most promising candidate of dark energy. Its definition is originally motivated from the entropy-area relation which depends on the theory of gravity under consideration. Recently a new definition of HDE is proposed with the help of quantum corrections to the entropy-area relation in the setup of loop quantum cosmology. Using this new definition, we investigate the model of interacting dark energy and derive its effective equation of state. Finally we establish a correspondence between generalized Chaplygin gas and entropy-corrected holographic dark energy.

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“…Gradually, it was found that interaction in the dark sector has many important outcomes. The presence of an interaction may push the dark energy equation of state to cross the phantom divide line [3,[58][59][60]. This is an interesting outcome in this context, because in order to explain the phantom crossing we need to introduce the negative sign before the kinetic term, which eventually invites instabilities both at the classical and quantum levels.…”

Section: Introductionmentioning

confidence: 99%

Theoretical and observational bounds on some interacting vacuum energy scenarios

et al. 2021

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The dynamics of interacting dark matter-dark energy models is characterized through an interaction rate function quantifying the energy flow between these dark sectors. In most of the interaction functions, the expansion rate Hubble function is considered and sometimes it is argued that, as the interaction function is a local property, the inclusion of the Hubble function may influence the overall dynamics. This is the starting point of the present article where we consider a very simple interacting cosmic scenario between vacuum energy and the cold dark matter characterized by various interaction functions originated from a general interaction function:, where ρ c , ρ x are respectively the cold dark matter density and vacuum energy density; α, β are real numbers and Γ is the coupling parameter with dimension equal to the dimension of the Hubble rate. We investigate four distinct interacting cosmic scenarios and constrain them both theoretically and observationally. Our analyses clearly reveal that the interaction models should be carefully handled.

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Thermodynamics second law and ω=−1 crossing(s) in interacting holographic dark energy model

Cited by 68 publications

References 56 publications

In the realm of the Hubble tension—a review of solutions ^*

In the realm of the Hubble tension—a review of solutions ^*

Interacting holographic dark energy with logarithmic correction

Theoretical and observational bounds on some interacting vacuum energy scenarios

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Thermodynamics second law and ω=−1 crossing(s) in interacting holographic dark energy model

Cited by 68 publications

References 56 publications

In the realm of the Hubble tension—a review of solutions *

In the realm of the Hubble tension—a review of solutions *

Interacting holographic dark energy with logarithmic correction

Theoretical and observational bounds on some interacting vacuum energy scenarios

Contact Info

Product

Resources

About

In the realm of the Hubble tension—a review of solutions ^*

In the realm of the Hubble tension—a review of solutions ^*