Abstract
We study the evolution of spatial curvature for thawing class of dark energy models. We examine the evolution of the equation of state parameter, wϕ, as a function of the scale factor a, for the case in which the scalar field ϕ evolve in nearly flat scalar potential. We show that all such models provide the corresponding approximate analytical expressions for wϕ(Ωϕ,Ωk) and wϕ(a). We present observational constraints on these models.
Highlights
We study the evolution of spatial curvature for thawing class of dark energy models
The astronomical measurements showed that Type Ia SNe at a redshift of z ∼ 0.5 were systematically fainted which could be attributed to an acceleration of the universe caused by a non-zero vacuum energy density
Since the evolution of the quintessence scalar field my be described by the change of the equation of state parameter wφ, so that we could distinguish two possible situations: the case in which dωφ/dφ < 0 and dωφ/dφ > 0
Summary
Current measurements of redshift and luminosity-distance relations of Type Ia Supernovae (SNe)[1] indicate that the expansion of the universe presents an accelerated phase [2, 3]. The astronomical measurements showed that Type Ia SNe at a redshift of z ∼ 0.5 were systematically fainted which could be attributed to an acceleration of the universe caused by a non-zero vacuum energy density. Since the evolution of the quintessence scalar field my be described by the change of the equation of state parameter wφ, so that we could distinguish two possible situations: the case in which dωφ/dφ < 0 and dωφ/dφ > 0. The former case is referred as the freezing and the later the thawing scenarios, respectively[22](see Ref.
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