Curvature of the universe and the dark energy potential

Abstract

The flatness of an accelerating universe model (characterized by a dark energy scalar field $\chi$) is mimicked from a curved model that is filled with, apart from the cold dark matter component, a quintessencelike scalar field $Q$. In this process, we characterize the original scalar potential $V(Q)$ and the mimicked scalar potential $V(\chi )$ associated to the scalar fields $Q$ and $\chi$, respectively. The parameters of the original model are fixed through the mimicked quantities that we relate to the present astronomical data, such that the equation state parameter $w_{{}_{\chi }}$ and the dark energy density parameter ${\Omega }_{\chi }$.

References 7 and 8 have been corrected: (7) Riess et al. 1998, AJ, 116, 1009 and (8) Perlmutter et al. 1999, ApJ, 517, 565

Cited by in corpus (3)

• Accelerated closed universes in scalar-tensor theories
• An accelerated closed universe
• Curvature in causal BD-type inflationary cosmology