Masashi Suwa | Searcharxiv

arXiv2015

The interacting generalized Ricci dark energy model in non-flat universe

We extend our previous analysis and consider the interacting holographic Ricci dark energy (IRDE) model in non-flat universe. We study astrophysical constraints on this model using the recent observations including the type Ia supernovae (SNIa), the baryon acoustic oscillation (BAO), the cosmic microwave background (CMB) anisotropy, and the Hubble parameter. It is shown that the allowed parameter range for the fractional energy density of the curvature is $-0.005$ $\lesssim$ $Ω_{k0}$ $\lesssim$ $0.015$ in the presence of the interactions between dark energy and matter. Without the interaction, the flat universe is observationally disfavored in this model.

astro-ph.CO↗

arXiv2010

Observational constraints on the interacting Ricci dark energy model

We consider an extension of the holographic Ricci dark energy model by introducing an interaction between dark energy and matter. In this model, the dark energy density is given by $rho_{Lambda}=-frac{1}{2}alpha M_{p}^{2}{R}$, where ${R}$ is the Ricci scalar curvature, $M_{p}$ is the reduced Planck mass, and $alpha$ is a dimensionless parameter. The interaction rate is given by $Q=gamma H rho_{Lambda}$, where $H$ is the Hubble expansion rate, and $gamma$ is a dimensionless parameter. We investigate current observational constraints on this model by applying the type Ia supernovae, the baryon acoustic oscillation and the CMB anisotropy data. It is shown that a nonvanishing interaction rate is favored by the observations. The best fit values are $alpha=0.45 pm 0.03$ and $gamma=0.15 pm 0.03$ for the present dark energy density parameter $Omega_{Lambda 0}=0.73 pm0.03$.

astro-ph.CO↗