2008/01/31 by Khamphee Karwan
Physics and Astronomy · #Black Holes and Theoretical Physics #Cosmology and Gravitation Theories #Galaxies: Formation, Evolution, Phenomena #astro-ph
paper · pdf · doi:10.1088/1475-7516/2008/05/011
published as JCAP0805:011,2008 · 16 pages, 5 figures; revised version to appear in JCAP; references added
openalex publication_date 2008/05/13 · arxiv created 2008/05/14 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/30
We study the dynamical behaviour of the interacting holographic dark energy model whose interaction term is Q = 3 H (λ d ρ d +λ c ρ c ), where ρ d and ρ c are the energy densities of dark energy and cold dark matter respectively. To satisfy the observational constraints from type Ia supernovae, the cosmic microwave background shift parameter and baryon acoustic oscillation measurements, if λ c = λ d or λ d ,λ c >0, the cosmic evolution will only reach the attractor in the future and the ratio ρ c /ρ d cannot be slowly varying at present. Since the cosmic attractor can be reached in the future even when the present values of the cosmological parameters do not satisfy the observational constraints, the coincidence problem is not really alleviated in this case. However, if and they are allowed to be negative, the ratio ρ c /ρ d can be slowly varying at present and the cosmic attractor can be reached near the present epoch. Hence, the alleviation of the coincidence problem is attainable in this case. The alleviation of the coincidence problem in this case is still attainable when confronting this model with Sloan Digital Sky Survey data.