Holographic energy density on Hořava-Lifshitz cosmology

Abstract

In Hořava-Lifshitz cosmology we use the holographic Ricci-like cut-off for the energy density proposed by L. N. Granda and A. Oliveros and under this framework we study, through the cosmic evolution at late times, the sign change in the amount of non-conservation energy ($Q$) present in this cosmology. We revise the early stage (curvature-dependent) of this cosmology, where a term reminiscent of stiff matter is the dominant, and in this stage we find a power-law solution for the cosmic scale factor although $\omega =-1$. Late and early phantom schemes are obtained without requiring $\omega <-1$. Nevertheless, these schemes are not feasible according to what is shown in this paper. We also show that $\omega =-1$ alone does not imply a de Sitter phase in the present cosmology. Thermal aspects are revised by considering the energy interchange between the bulk and the spacetime boundary and we conclude that there is no thermal equilibrium between them. Finally, a ghost scalar graviton (extra degree of freedom in HL gravity) is required by the observational data.

arXiv comment8 pages, 3 figures, Published in PRD

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Cited by in corpus (4)

• On sign-changeable interaction in FLRW cosmology
• Interacting cosmic fluids and phase transitions under a holographic modeling for dark energy
• Bulk-Boundary interaction and the second law in Hořava-Lifshitz cosmology
• Gauss-Bonnet dark energy on Hořava-Lifshitz cosmology