Supernova constraints on a holographic dark energy model

Huang, Qing-Guo; Gong, Yungui

doi:10.1088/1475-7516/2004/08/006

Cited by 279 publications

(214 citation statements)

References 23 publications

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“…Recently, some constraints from SNe Ia on related model where obtained in Refs. [16,17]. In this paper, we extend the analysis carried out in Ref.…”

Section: Introductionmentioning

confidence: 57%

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Constraints on holographic dark energy from type Ia supernova observations

2005

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In this paper, we use the type Ia supernovae data to constrain the holographic dark energy model proposed by Li. We also apply a cosmic age test to this analysis. We consider in this paper a spatially flat Friedmann-RobertsonWalker Universe with matter component and holographic dark energy component. The fit result shows that the case c < 1 (c = 0.21) is favored, which implies that the holographic dark energy behaves as a quintom-type dark energy. Furthermore, we also perform a joint analysis of SNe+CMB+LSS to this model; the result is well improved, and still upholds the quintom dark energy conclusion. The best fit results in our analysis are c = 0.81, Ω 0 m = 0.28, and h = 0.65, which lead to the present equation of state of dark energy w 0 = −1.03 and the deceleration/acceleration transition redshift z T = 0.63. Finally, an expected SNAP simulation using ΛCDM as a fiducial model is performed on this model, and the result shows that the holographic dark energy model takes on c < 1 (c = 0.92) even though the dark energy is indeed a cosmological constant.

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“…Recently, some constraints from SNe Ia on related model where obtained in Refs. [16,17]. In this paper, we extend the analysis carried out in Ref.…”

Section: Introductionmentioning

confidence: 57%

“…Some speculations on the deep reasons of the holographic dark energy were considered by several authors [14]; further studies on this model see also [15][16][17][18][19][20][21][22][23].…”

Section: Introductionmentioning

confidence: 99%

Constraints on holographic dark energy from type Ia supernova observations

2005

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“…We assumed two different phases of HDE model i.e., quintessence regime (c 1) and phantom regime (c < 1). In the case of phantom regime, we adopted the constrained value for the model parameter c = 0.815 obtained in Enqvist & Sloth (2004); Gong (2004); Huang & Gong (2004b); Huang & Li (2004); Li et al (2009). We first investigated the growth of structures in linear regime and showed that the growth of density perturbations g(a) is slowed down in HDE models compared to the EdS and ΛCDM models due to a larger Hubble parameter.…”

Section: Discussionmentioning

confidence: 99%

“…Using recent observational data, the value of the holographic parameter c in a flat Universe was constrained to c = 0.815 +0.179 −0.139 (Enqvist & Sloth 2004;Gong 2004;Huang & Gong 2004b;Huang & Li 2004;Li et al 2009). The cosmic coincidence problem can be solved by inflation in HDE model (Li 2004).…”

Section: Cosmology With Holographic Dark Energymentioning

confidence: 99%

Evolution of spherical overdensities in holographic dark energy models

Naderi¹,

Malekjani²,

Pace³

2015

Monthly Notices of the Royal Astronomical Society

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In this work we investigate the spherical collapse model in flat FRW dark energy universes. We consider the Holographic Dark Energy (HDE) model as a dynamical dark energy scenario with a slowly time-varying equation-of-state (EoS) parameter w de in order to evaluate the effects of the dark energy component on structure formation in the universe. We first calculate the evolution of density perturbations in the linear regime for both phantom and quintessence behavior of the HDE model and compare the results with standard Einstein-de Sitter (EdS) and ΛCDM models. We then calculate the evolution of two characterizing parameters in the spherical collapse model, i.e., the linear density threshold δ c and the virial overdensity parameter ∆ vir . We show that in HDE cosmologies the growth factor g(a) and the linear overdensity parameter δ c fall behind the values for a ΛCDM universe while the virial overdensity ∆ vir is larger in HDE models than in the ΛCDM model. We also show that the ratio between the radius of the spherical perturbations at the virialization and turn-around time is smaller in HDE cosmologies than that predicted in a ΛCDM universe. Hence the growth of structures starts earlier in HDE models than in ΛCDM cosmologies and more concentrated objects can form in this case. It has been shown that the non-vanishing surface pressure leads to smaller virial radius and larger virial overdensity ∆ vir . We compare the predicted number of halos in HDE cosmologies and find out that in general this value is smaller than for ΛCDM models at higher redshifts and we compare different mass function prescriptions. Finally, we compare the results of the HDE models with observations.

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“…We shall focus on the DE model inspired by the holographic idea that the energy within our horizon cannot exceed the mass of a black hole of the same size [26,27,28]. The extension of the holographic principle to a general cosmological setting was first addressed by Fischler and Susskind [29] and subsequently got modified by many authors [30]- [34].…”

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confidence: 99%

Thermodynamical description of the interaction between holographic dark energy and dark matter

et al. 2008

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We present a thermodynamical description of the interaction between holographic dark energy and dark matter. If holographic dark energy and dark matter evolve separately, each of them remains in thermodynamic equilibrium. A small interaction between them may be viewed as a stable thermal fluctuation that brings a logarithmic correction to the equilibrium entropy. From this correction we obtain a physical expression for the interaction which is consistent with phenomenological descriptions and passes reasonably well the observational tests.

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Supernova constraints on a holographic dark energy model

Cited by 279 publications

References 23 publications

Constraints on holographic dark energy from type Ia supernova observations

Constraints on holographic dark energy from type Ia supernova observations

Evolution of spherical overdensities in holographic dark energy models

Thermodynamical description of the interaction between holographic dark energy and dark matter

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