2008/01/31 by M. R. Setare, Elias C. Vagenas · 8 citations
Physics and Astronomy · #Black Holes and Theoretical Physics #Cosmology and Gravitation Theories #Galaxies: Formation, Evolution, Phenomena #astro-ph #gr-qc #hep-th
paper · pdf · doi:10.1016/j.physletb.2008.07.013
published as Phys.Lett.B666:111-115,2008 · 12 pages, no figure, LaTeX; v2: 13 pages now, comments and clarifications added, to appear in Phys. Lett. B
arxiv created 2008/07/09 · openalex publication_date 2008/07/14 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/31
Motivated by the recent work of Wang, Lin, Pavon, and Abdalla [B. Wang, C.Y. Lin, D. Pavon, E. Abdalla, Phys. Lett. B 662 (2008) 1, arXiv: 0711.2214 [hep-th]], we generalize their work to the non-flat case. In particular, we provide a thermodynamical interpretation for the holographic dark energy model in a non-flat universe. For this case, the characteristic length is no more the radius of the event horizon (RE) but the event horizon radius as measured from the sphere of the horizon (L). Furthermore, when interaction between the dark components of the holographic dark energy model in the non-flat universe is present its thermodynamical interpretation changes by a stable thermal fluctuation. A relation between the interaction term of the dark components and this thermal fluctuation is obtained. In the limiting case of a flat universe, i.e. k=0, all results given in [B. Wang, C.Y. Lin, D. Pavon, E. Abdalla, Phys. Lett. B 662 (2008) 1, arXiv: 0711.2214 [hep-th]] are obtained.