Cosmology with Ricci dark energy

Abstract

We assume the cosmological dark sector to consist of pressureless matter and holographic dark energy with a cutoff length proportional to the Ricci scale. The requirement of separate energy-momentum conservation of the components is shown to establish a relation between the matter fraction and the (necessarily time-dependent) equation-of-state parameter of the dark energy. Focusing on intrinsically adiabatic pressure perturbations of the dark-energy component, the matter perturbations are found as linear combinations of the total energy-density perturbations of the cosmic medium and the relative (nonadiabatic) perturbations of the components. The resulting background dynamics is consistent with observations from supernovae of type Ia, baryonic acoustic oscillations and the differential age of old objects. The perturbation dynamics, on the other hand, is plagued by instabilities which excludes any phantom-type equation of state. The only stable configuration is singled out by a fixed relation between the present matter fraction ${\Omega }_{m0}$ and the present value ${\omega }_0$ of the equation-of-state parameter of the dark energy. However, this instability-avoiding configuration is only marginally consistent with the observationally preferred background values of the mentioned parameters.

29 pages, 8 figures, new material and new results added, conclusions enlarged and sharpened, references added, to appear in PRD

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• Interacting Ricci-like holographic dark energy
• Holographic dark energy: constraints on the interaction from diverse observational data sets
• An effective quintessence field with a power-law potential
• Quantisation of the holographic Ricci dark energy model
• Instability in interacting dark sector: An appropriate Holographic Ricci dark energy model
• Bayesian Comparison of Interacting Modified Holographic Ricci Dark Energy Scenarios
• Israel-Stewart approach to viscous dissipative extended holographic Ricci dark energy dominated universe
• Can Holographic dark energy increase the mass of the wormhole?
• Thermodynamics of interacting holographic dark energy
• Matter Growth in Imperfect Fluid Cosmology
• Barrow holographic dark energy interacting model in the presence of radiation and matter
• A bound system in the expanding universe with modified holographic Ricci dark energy and dark matter
• Ricci-Cubic Holographic Dark Energy: Confronting Observations, Stability and the Cosmic Coincidence Problem
• Semi-holographic model revisited
• Matter growth in extended $\Lambda$CDM cosmology
• Late-time cosmological constraints on three holographic dark energy models with DESI DR2 BAO and Type Ia supernovae