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Transition of the dark energy equation of state in an interacting holographic dark energy model
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abstract
A model of holographic dark energy with an interaction with matter fields has been investigated. Choosing the future event horizon as an IR cutoff, we have shown that the ratio of energy densities can vary with time. With the interaction between the two different constituents of the universe, we observed the evolution of the universe, from early deceleration to late time acceleration. In addition, we have found that such an interacting dark energy model can accommodate a transition of the dark energy from a normal state where $w_D>-1$ to $w_D<-1$ phantom regimes. Implications of interacting dark energy model for the observation of dark energy transition has been discussed.
Forward citations
Cited by 13 Pith papers
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A comprehensive numerical study on four categories of holographic dark energy models
Seven holographic dark energy models are constrained with DESI BAO, Planck CMB, and PantheonPlus supernovae; LambdaCDM stays preferred, Ricci dark energy is ruled out, and event-horizon models show large data-set-depe...
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Holographic bounce
Holographic infrared and ultraviolet cutoffs can produce bouncing solutions, including nonsingular ones, and can be designed to reproduce F(R) gravity bounce.
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Interacting Dark Sector field theory with phantom crossing
An interacting dark sector model with Yukawa-coupled fermionic DM and Born-Infeld tachyonic scalar produces recent double phantom crossing in effective w_DE, fits DESI+Planck+SN data, and predicts ultralight DM mass o...
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Constraints on Barrow and Tsallis Holographic Dark Energy from DESI DR2 BAO data
Barrow and Tsallis holographic dark energy models fit DESI DR2 data but are disfavored by information criteria versus LambdaCDM and do not ease the Hubble tension.
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Topological dark energy from black-hole formations and mergers through the gravity-thermodynamics approach
Black hole formation and merger, through topology changes of the cosmic apparent horizon, generate an effective dark energy whose equation of state is phantom-like or quintessence-like depending on the sign of the Gau...
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Interacting phantom dark energy: new accelerating scaling attractors
Interacting phantom dark energy with two previously underused potentials admits new stable late-time accelerating solutions in which dark matter and dark energy coexist.
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Revisiting the Hubble tension problem in the framework of holographic dark energy
HDE models with future event horizon IR cutoff partially ease the Hubble tension while Hubble-scale cutoffs do not, consistent across six models and multiple BAO/SN/CMB combinations.
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Solving an Interacting Quintessence Model with a Sound Horizon Initial Condition and its Observational Constraints
An interacting quintessence model with initial conditions set by the CMB sound horizon angle increases H0 with coupling strength, but observational constraints show it does not resolve the H0 or S8 tensions.
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In search of an interaction in the dark sector through Gaussian Process and ANN approaches
Reconstructed dark-sector interaction from CC and Pantheon+ data is consistent with zero for w_DE = -1 but becomes nonzero whenever w_DE is fixed away from -1, in both Gaussian Process and ANN analyses.
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Dissipative Cosmology and the Nature of Dark Energy: Insights from Bulk Viscosity with DESI DR2 observations
Bulk viscous fluid models for dark energy yield improved fits to supernova, BAO, and CMB data over LambdaCDM, especially in the interacting non-minimal case.
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The Quintom theory of dark energy after DESI DR2
This review traces the history of dynamical dark energy, presents the no-go theorem against single-field crossing of w = -1, and surveys viable Quintom constructions including multi-field models and modified gravity i...
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A short review on Quintom dark energy theory
Quintom dark energy models permit the equation of state to cross w=-1, supporting bouncing cosmologies and CMB-based tests of dark energy nature.
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Exploring Hubble Tension Alleviation through Neutrino-Coupled Perturbed $f(R)$ Gravity
A fit of Hu-Sawicki f(R) gravity with a fitted neutrino interaction to CMB, lensing, BAO, CC, and Pantheon data returns H0 near 70 km/s/Mpc, partially easing but not resolving the Hubble and S8 tensions.
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