Holographic energy density on Hořava-Lifshitz cosmology

Samuel Lepe, Francisco Peña, and Francisco Torres
Phys. Rev. D 91, 024023 – Published 14 January 2015

Abstract

In Hořava-Lifshitz cosmology we use the holographic Ricci-like cutoff 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 nonconservation 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 ω=1. Late and early phantom schemes are obtained without requiring ω<1. Nevertheless, these schemes are not feasible according to what is shown in this paper. We also show that ω=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.

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  • Received 29 October 2014

DOI:https://doi.org/10.1103/PhysRevD.91.024023

© 2015 American Physical Society

Authors & Affiliations

Samuel Lepe1,*, Francisco Peña2,†, and Francisco Torres1,‡

  • 1Instituto de Física, Facultad de Ciencias, Pontificia Universidad Católica de Valparaíso, Avenida Brasil 4950, Valparaíso, Chile
  • 2Departamento de Ciencias Físicas, Facultad de Ingeniería y Ciencias, Universidad de La Frontera, Casilla 54-D, Temuco, Chile

  • *slepe@ucv.cl
  • francisco.pena@ufrontera.cl
  • francisco.t2@gmail.com

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Issue

Vol. 91, Iss. 2 — 15 January 2015

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