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Interacting ghost dark energy in non-flat universe. (English) Zbl 1235.85012

Summary: A new dark energy model called “ghost dark energy” was recently suggested to explain the observed accelerating expansion of the universe. This model originates from the Veneziano ghost of QCD. The dark energy density is proportional to Hubble parameter, \(\rho_{D } = \alpha H\), where \(\alpha\) is a constant of order \(\Lambda_{\text{QCD}}^3\) and \(\Lambda_{\text{QCD}} \sim 100 \text{MeV}\) is QCD mass scale. In this Letter, we extend the ghost dark energy model to the universe with spatial curvature in the presence of interaction between dark matter and dark energy. We study cosmological implications of this model in detail. In the absence of interaction the equation of state parameter of ghost dark energy is always \(w_{D} > -1\) and mimics a cosmological constant in the late time, while it is possible to have \(w_{D} < -1\) provided the interaction is taken into account. When \(k = 0\), all previous results of ghost dark energy in flat universe are recovered. For the observational test, we use Supernova type Ia Gold sample, shift parameter of cosmic microwave background radiation and the correlation of acoustic oscillation on the last scattering surface and the baryonic acoustic peak from Sloan Digital Sky Survey are used to confine the value of free parameter of mentioned model.

MSC:

85A40 Astrophysical cosmology
83F05 Relativistic cosmology
83C55 Macroscopic interaction of the gravitational field with matter (hydrodynamics, etc.)
81V05 Strong interaction, including quantum chromodynamics
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