Kaniadakis holographic dark energy in Brans–Dicke cosmology

Ghaffari, S.

doi:10.1142/s0217732322501528

Cited by 15 publications

(16 citation statements)

References 96 publications

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“…However, since radiation effects are dominant in the early Universe only, we expect they do not spoil considerably our predictions for the current and future epochs. Additionally, we aim at investigating the correspondence between our model and HDE based on other extensions of Boltzmann-Gibbs entropy, such as Tsallis [59,[80][81][82][83] and Kaniadakis [60] holographic dark energy. Also, interesting results could be found by connecting BHDE and dark energy model based on Gurzadyan-Xue framework.…”

Section: Discussionmentioning

confidence: 99%

“…In [24], the authors have shown that the non-interacting HDE with the Hubble radius as IR cutoff cannot explain the current accelerated expansion of Universe in the BD theory. While in a similar analysis, it has been shown that the Tsallis and Kaniadakis holographic dark energy, due to the generalized entropy, with the Hubble cutoff in the BD gravity, can lead the accelerated Universe phase, even in the absence of interaction between two dark sectors [59,60].…”

Section: Introductionmentioning

confidence: 90%

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Barrow holographic dark energy in the Brans–Dicke cosmology

2023

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We construct a holographic model for dark energy in the Brans–Dicke cosmology by using the holographic principle considering the Barrow entropy instead of the standard Bekenstein–Hawking one. The former arises from the effort to account for quantum gravitational effects in black hole physics and, according to the gravity–thermodynamic conjecture, in the cosmological framework. In order to explore the cosmological consequences of our model, we consider the Hubble horizon as the IR cutoff. We investigate both the non-interacting and interacting cases with the sign-changeable and linear interactions, showing that they can explain the present accelerated phase of the Universe expansion, in contrast to the standard holographic dark energy model. We then perform the stability analysis according to the squared sound speed. We find that, while the non-interacting model is unstable against small perturbations, the sign-changeable interacting one can be stable only for suitable values of the model parameters. On the other hand, the linear interacting model always predicts a stable Universe. The consistency of the model with respect to cosmological observations is discussed.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 90%

Barrow holographic dark energy in the Brans–Dicke cosmology

2023

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“…For our next purposes, it is now convenient to rewrite the modified Friedmann Equation (35) in the equivalent form…”

Section: Big Bang Nucleosynthesis In Kaniadakis Statisticsmentioning

confidence: 99%

“…The standard HDE scenario is built upon Bekenstein–Hawking entropy, which arises as the black hole application of the BGS one. However, in [ 13 , 14 , 15 , 32 ], a generalized HDE based on Kaniadakis entropy has been investigated along with its implications on the cosmic evolution and thermal properties of the Universe (see also [ 23 , 24 , 33 , 34 , 35 ] for further applications). Remarkably, it has been shown that Kaniadakis dark energy exhibits peculiar features that do not have any correspondence in the traditional HDE, potentially providing a way to alleviate the Hubble tension.…”

Section: Introductionmentioning

confidence: 99%

Gravity and Cosmology in Kaniadakis Statistics: Current Status and Future Challenges

Luciano

2022

Entropy

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Kaniadakis statistics is a widespread paradigm to describe complex systems in the relativistic realm. Recently, gravitational and cosmological scenarios based on Kaniadakis (κ-deformed) entropy have been considered, leading to generalized models that predict a richer phenomenology comparing to their standard Maxwell–Boltzmann counterparts. The purpose of the present effort is to explore recent advances and future challenges of Gravity and Cosmology in Kaniadakis statistics. More specifically, the first part of the work contains a review of κ-entropy implications on Holographic Dark Energy, Entropic Gravity, Black hole thermodynamics and Loop Quantum Gravity, among others. In the second part, we focus on the study of Big Bang Nucleosynthesis in Kaniadakis Cosmology. By demanding consistency between theoretical predictions of our model and observational measurements of freeze-out temperature fluctuations and primordial abundances of 4He and D, we constrain the free κ-parameter, discussing to what extent the Kaniadakis framework can provide a successful description of the observed Universe.

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“…Each of these models is examined in different structures and conditions. The results are evaluated and compared with the latest observable data [41][42][43]. As mentioned, one of the most famous models in describing the nature of dark energy is a scalar field theory called quintessence, which represents a scalar field with a parameter (Q) and a decreasing potential.…”

Section: Introductionmentioning

confidence: 99%

Tsallis holographic dark energy under complex form of quintessence model

Sadeghi¹,

Gashti²,

Azizi³

2023

Commun. Theor. Phys.

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In this paper, we use a Tsallis holographic dark energy model in two forms, interacting and non-interacting cases, to acquire some parameters as the equation of state for the energy density of the Tsallis model in the FRW universe concerning the complex form of quintessence model. We will study the cosmology of complex quintessence by revamping the potential and investigating the scalar field dynamics. Then we analyze ($\omega-\omega'$) and stability in two cases, i.e., non-interacting and interacting. We will explore whether these cases describe a real universe by calculating fractional energy density $\Omega_{D}$ and concerning two parts of the quintessence field effect ( complex and real part ) by considering the real part of this field to be a slow-roll field. We know that the part in which the fractional energy density ($\Omega_{D} > 1$) does not describe a real universe. Also, we specified an interacting coupling parameter $b^{2}$ that depends on the constant parameter of the Tsallis holographic model ($\delta$) with respect to fractional energy density ($0.73$). Unlike independence between the fractional energy density and interacting coupling in the real quintessence model, we determine a relationship among these parameters in this theory. Finally, by plotting some figures, we specify the features of ($\omega-\omega'$) and ($\nu_{s}^{2}$) in two cases and compare the result with each other

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Kaniadakis holographic dark energy in Brans–Dicke cosmology

Cited by 15 publications

References 96 publications

Barrow holographic dark energy in the Brans–Dicke cosmology

Barrow holographic dark energy in the Brans–Dicke cosmology

Gravity and Cosmology in Kaniadakis Statistics: Current Status and Future Challenges

Tsallis holographic dark energy under complex form of quintessence model

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