Cosmic evolution and thermal stability of Barrow holographic dark energy in a nonflat Friedmann-Robertson-Walker Universe

Luciano, Giuseppe Gaetano

doi:10.1103/physrevd.106.083530

Cited by 28 publications

(4 citation statements)

References 74 publications

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“…Holographic Dark Energy is a dynamical model of dark energy built on the usage of the holographic principle and Bekenstein–Hawking area law. Although cosmological applications of HDE have been extensively considered in the past literature [ 46 , 47 , 48 ], its shortcomings in reproducing the thermal history of the Universe have motivated some tentative changes over the years [ 14 , 15 , 49 , 50 , 51 , 52 , 53 ]. Among these generalizations, promising results have been provided by HDE based on Kaniadakis entropy (Kaniadakis Holographic Dark Energy, KHDE).…”

Section: Gravity and Cosmology In Kaniadakis Statistical Theory: Rece...mentioning

confidence: 99%

“…The resulting mechanics has attracted growing interest in the last decades, particularly due to its capability to address the area-scaling problem of black hole entropy [2]. A similar deformation occurs in Barrow model [3], motivated by a quantum gravitational (fractal-like) structure of the horizon geometry of black holes (see also [4,5] for applications to Cosmology), while a power-law corrected entropy appears in [6,7] inspired by the idea that the origin of black-hole entropy may lie in the entanglement of quantum fields between inside and outside of the horizon.…”

Section: Introductionmentioning

confidence: 96%

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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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Section: Gravity and Cosmology In Kaniadakis Statistical Theory: Rece...mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 96%

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

Luciano

2022

Entropy

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“…Quantum gravity effects are parameterized by the Barrow exponent 0 ≤ ≤ 1, with 0 giving the BH limit, while 1 corresponding to the maximal entropy deformation. It is worth mentioning that cosmological constraints on have been inferred in [48][49][50][51][52][53][54][55][56][57]. The possibility for a running has also been discussed in [58].…”

Section: Introductionmentioning

confidence: 99%

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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“…Despite the intensive study, the shortcomings of the HDE in describing the history of a flat Friedmann-Robertson-Walker (FRW) universe have prompted tentative changes to this approach. For instance, HDE has been used to address the DE problem in Brans-Dicke Cosmology [36][37][38][39][40][41][42] by considering different IR cutoffs [28,29,41] or and/or generalized entropies [43][44][45][46][47][48][49][50][51][52][53][54][55][56][57][58]. In particular, the latter path has led to promising models, such as Tsallis [43][44][45][46]59], Barrow [47,51,53], and Kaniadakis [49,50,52] holographic dark energy, the latter two being motivated by quantum gravitational and relativistic considerations, respectively.…”

Section: Introductionmentioning

confidence: 99%

Lagrangian Reconstruction of Barrow Holographic Dark Energy in Interacting Tachyon Model

Luciano

Liu

2023

Symmetry

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We consider a correspondence between the tachyon dark energy model and Barrow holographic dark energy (BHDE). The latter is a modified scenario based on the application of the holographic principle with Barrow entropy instead of the usual Bekenstein–Hawking one. We reconstruct the dynamics of the tachyon scalar field T in a curved Friedmann–Robertson–Walker universe both in the presence and absence of interactions between dark energy and matter. As a result, we show that the tachyon field exhibits non-trivial dynamics. In a flat universe, T˙2 must always be vanishing, independently of the existence of interaction. This implies ωD=−1 for the equation-of-state parameter, which in turn can be used for modeling the cosmological constant behavior. On the other hand, for a non-flat universe and various values of the Barrow parameter, we find that T˙2 decreases monotonically for increasing cos(Rh/a) and cosh(Rh/a), where Rh and a are the future event horizon and the scale factor, respectively. Specifically, T˙2≥0 for a closed universe, while T˙2<0 for an open one, which is physically not allowed. We finally comment on the inflation mechanism and trans-Planckian censorship conjecture in BHDE and discuss observational consistency of our model.

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Cosmic evolution and thermal stability of Barrow holographic dark energy in a nonflat Friedmann-Robertson-Walker Universe

Cited by 28 publications

References 74 publications

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

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

Barrow holographic dark energy in the Brans–Dicke cosmology

Lagrangian Reconstruction of Barrow Holographic Dark Energy in Interacting Tachyon Model

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