Interacting dark energy, holographic principle, and coincidence problem

The holographic dark energy model is proposed by Li as an attempt for probing the nature of dark energy within the framework of quantum gravity. The main characteristic of holographic dark energy is governed by a numerical parameter c in the model. The parameter c can only be determined by observations. Thus, in order to characterize the evolving feature of dark energy and to predict the fate of the universe, it is of extraordinary importance to constrain the parameter c by using the currently available observational data. In this paper, we derive constraints on the holographic dark energy model from the latest observational data including the gold sample of 182 Type Ia supernovae (SNIa), the shift parameter of the cosmic microwave background (CMB) given by the three-year Wilkinson Microwave Anisotropy Probe (WMAP) observations, and the baryon acoustic oscillation (BAO) measurement from the Sloan Digital Sky Survey (SDSS). The joint analysis gives the fit results in 1-σ: c = 0.91 +0.26 −0.18 and Ω m0 = 0.29 ± 0.03. That is to say, though the possibility of c < 1 is more favored, the possibility of c > 1 can not be excluded in one-sigma error range, which is somewhat different from the result derived from previous investigations using earlier data. So, according to the new data, the evidence for the quintom feature in the holographic dark energy model is not as strong as before.

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“…For extensive studies on the holographic dark energy model see e.g. [47,48,49,50,51,52,53,54,55,56,57,58,59].…”

Section: Introductionmentioning

confidence: 99%

Constraints on holographic dark energy from the latest supernovae, galaxy clustering, and cosmic microwave background anisotropy observations

Zhang

2007

Phys. Rev. D

204

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“…Quite interestingly, it was reported in [8] that if dark energy and dark matter are allowed to interact non-gravitationally with each other, the coincidence problem can be solved. Following this, a series of works with coupled dark matter and dark energy arXiv:1808.01669v1 [gr-qc] 5 Aug 2018 had the same conclusions [9,10,11,12,13]. However, some recent results fueled the investigations of coupled dark matter and dark energy with the claim that the observational data favor an interaction in the dark sector [14,15,16,17,18,19,20,21,22,23].…”

Section: Introductionmentioning

confidence: 90%

Large-scale (in) stability analysis of an exactly solved coupled dark-energy model

et al. 2018

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Assuming a non-gravitational interaction amongst the dark fluids of our universe namely, the dark matter and dark energy, we study a specific interaction model in the background of a spatially flat Friedmann-Lemaître-Robertson-Walker geometry. The interaction model, as we found, solves the background evolution in an analytic way when the dark energy takes a constant barotropic equation of state, wx. In particular, we analyze two separate interaction scenarios, namely, when the dark energy is a fluid other than the vacuum energy (i.e., wx = −1) and when it is vacuum energy itself (i.e., wx = −1). We found that the interacting model with wx = −1 produces stable perturbation at large scales for wx < −1 with the coupling strength ξ < 0. Both the scenarios have been constrained with the latest astronomical data having distinct origin. The analyses show that a very small interaction with coupling strength is allowed and within 68.3% confidence-region, ξ = 0 is recovered. The analyses further show that a large coupling strength significantly affects the large scale dynamics of the universe while according to the observational data the interaction models are very well consistent with the Λ-cosmology. Furthermore, we observe that for the vacuum interaction scenario, the tension on H0 is not released while for the interacting dark energy scenario with wx < −1, the tension on H0 seems to be released partially because of the high error bars in H0. Finally, we close the work with the Bayesian evidence which shows that the ΛCDM cosmology is favored over the two interacting scenarios. 95.35.+d, 95.36.+x, 98.80.Es.

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“…Such coincidence problem led to another class of cosmological theories which is the theory of non-gravitational interaction between dark matter and dark energy. The non-gravitational interaction in the dark sector, precisely between dark matter and dark energy is a phenomenological concept that was originally thought to explain the different values of the time-independent cosmological constant [2], but later on, such concept was found to be very useful to explain the cosmic coincidence problem [9][10][11][12][13][14]. Certainly, this led to a large amount of investigations towards this direction where the dark sectors have direct interaction (also see [38][39][40][41][42][43][44][45]).…”

Section: Introductionmentioning

confidence: 99%

Effects of anisotropic stress in interacting dark matter – dark energy scenarios

Yang

Pan

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We study a novel interacting dark energy − dark matter scenario where the anisotropic stress of the large scale inhomogeneities is considered. The dark energy has a constant equation of state and the interaction model produces stable perturbations. The resulting picture is constrained using different astronomical data aiming to measure the impact of the anisotropic stress on the cosmological parameters. Our analyses show that a non-zero interaction in the dark sector is allowed while a non-interaction scenario is recovered within 68% CL. The anisotropic stress is also constrained to be small, and its zero value is permitted within 68% CL. The dark energy equation of state, wx, is also found to be close to '−1' boundary. However, from the ratio of the CMB TT spectra, we see that the model has a mild deviation from the ΛCDM cosmology while such deviation is almost forbidden from the CMB TT spectra alone. Although the deviation is not much significant, but from the present data, we cannot exclude such deviation. Overall, at the background level, the model is close to the ΛCDM cosmology while at the level of perturbations, a non-zero but a very small interaction in the dark sector is permitted. Perhaps, a more accurate conclusion can be made with the next generation of surveys. We also found that the region wx < −1, is found to be effective to release the tension on H0. Finally, from the Bayesian analysis, we find that ΛCDM remains in still preferred over the interacting scenarios.PACS numbers: 95.36.+x, 95.35.+d, 98.80.Es

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Interacting dark energy, holographic principle, and coincidence problem

Cited by 182 publications

References 59 publications

Constraints on holographic dark energy from the latest supernovae, galaxy clustering, and cosmic microwave background anisotropy observations

Constraints on holographic dark energy from the latest supernovae, galaxy clustering, and cosmic microwave background anisotropy observations

Large-scale (in) stability analysis of an exactly solved coupled dark-energy model

Effects of anisotropic stress in interacting dark matter – dark energy scenarios

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