Dynamical analysis and statefinder of Barrow holographic dark energy

Huang, Qihong; Huang, He; Xu, Bing; Tu, Feiquan; Chen, Jun

doi:10.1140/epjc/s10052-021-09480-3

Cited by 37 publications

(10 citation statements)

References 98 publications

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“…Hence, such a complex structure leads to a modification of the black hole entropy. This idea may have interesting consequences in cosmological and holographic applications [69][70][71][72][73][74][75][76][77][78][79][80]. Nevertheless, it also has interesting implications on the black hole properties itself, since it changes the black hole temperature too [81][82][83].…”

Section: Introductionmentioning

confidence: 99%

Constraints on Barrow Entropy from M87* and S2 Star Observations

et al. 2022

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We use data from M87* central black hole shadow, as well as from the S2 star observations, in order to extract constraints on Barrow entropy. The latter is a modified entropy arising from quantum-gravitational effects on the black hole horizon, quantified by the new parameter Δ. Such a change in entropy leads to a change in temperature, as well as to the properties of the black hole and its shadow. We investigate the photon sphere and the shadow of a black hole with Barrow entropy, and assuming a simple model for infalling and radiating gas we estimate the corresponding intensity. Furthermore, we use the radius in order to extract the real part of the quasinormal modes, and for completeness we investigate the spherical accretion of matter onto the black hole, focusing on isothermal and polytropic test fluids. We extract the allowed parameter region, and by applying a Monte-Carlo-Markov Chains analysis we find that Δ≃0.0036−0.0145+0.0792. Hence, our results place the upper bound Δ≲0.0828 at 1σ, a constraint that is less strong than the Big Bang Nucleosynthesis one, but significantly stronger than the late-time cosmological constraints.

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Section: Introductionmentioning

confidence: 99%

Constraints on Barrow Entropy from M87* and S2 Star Observations

et al. 2022

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“…where the matter contribution to the critical points is determined by the constraint (15). The existence and stability conditions of the critical points B 1 − B 3 are shown in Table 3, as well as the ω eff parameter.…”

Section: Case B: γ 1xmentioning

confidence: 99%

“…In Refs. [14,15] the authors apply dynamical systems methods and perform a statefinder analysis to interacting dark energy models. Even though the dynamical system analysis shows a similar asymptotic behavior for these models, the statefinder diagnosis allows to distinguish among models, when the evolution of the statefinder parameters is studied.…”

Section: Introductionmentioning

confidence: 99%

Dynamics and statefinder analysis of a class of sign-changeable interacting dark energy scenarios

Arévalo¹,

Cid²

2022

Preprint

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We revise the dynamical properties of a class of cosmological models where the dark sector interacts through an interacting term that changes sign during evolution. In particular, we obtain the critical points and we investigate the existence and stability conditions for cosmological solutions, describing radiation, matter and dark energy dominated eras. We find that all the studied models admit a stable critical point corresponding to an accelerated phase. We use background data to find the best fit parameters for one of the studied models, resulting an interacting parameter with a definite sign within 1σ confidence level, consistent with the results of the dynamical system analysis. We also compute the statefinder parameters and plot the r − q and r − s planes, where we observe different trajectories when we vary the interaction parameter for a specific model and when we vary the interacting scenario. We can in this sense distinguish among models, including ΛCDM.

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“…Furthermore, in [14] the authors used observational data from Supernovae (SNIa) Pantheon sample, as well as from direct measurements of the Hubble parameter from the cosmic chronometers (CC) sample, in order to extract constraints on the scenario of Barrow holographic dark energy. It is important to notice that the BHDE has been widely studied in the literature, e.g., [15][16][17][18][19][20][21][22][23][24][25][26].…”

Section: Introductionmentioning

confidence: 99%

Barrow holographic dark energy with Granda-Oliveros cut-off

Oliveros,

Sabogal,

Acero

2022

Preprint

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A study on the effects of implementing the Granda-Oliveros infrared cutoff in the recently introduced Barrow Holographic Dark Energy model is presented, and its cosmological evolution is investigated. We find how the deformation parameter, ∆, affects the values of H(z), and find that from this model it is possible to obtain an accelerated expansion regime of the universe at late times. We also obtain that increasing ∆ causes the EoS parameter to transition from quintessence to phantom. In addition, we show that the model can be used to describe the know eras of dominance. Finally, after studying the stability of the proposed model, a fit of the corresponding parameters is preformed, utilizing the measurements of the expansion rate of the universe, H(z). The best fit of the parameters is found to be (α, β, ∆) = (1.00 +0.02 −0.02 , 0.69 +0.03 −0.02 , 0.000 +0.004 −0.000 ) at 1σ C.L, for which the Bekenstein-Hawking relation is favored.

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Dynamical analysis and statefinder of Barrow holographic dark energy

Cited by 37 publications

References 98 publications

Constraints on Barrow Entropy from M87* and S2 Star Observations

Constraints on Barrow Entropy from M87* and S2 Star Observations

Dynamics and statefinder analysis of a class of sign-changeable interacting dark energy scenarios

Barrow holographic dark energy with Granda-Oliveros cut-off

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