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• W3100252661 startingPage "016" @default.
• W3100252661 abstract "We consider the viability of dark energy (DE) models in the framework of the scalar-tensor theory of gravity, including the possibility to have a phantom DE at small redshifts $z$ as admitted by supernova luminosity-distance data. For small $z$, the generic solution for these models is constructed in the form of a power series in $z$ without any approximation. Necessary constraints for DE to be phantom today and to cross the phantom divide line $p=-rho$ at small $z$ are presented. Considering the Solar System constraints, we find for the post-Newtonian parameters that $gamma_{PN}<1$ and $gamma_{PN,0}approx 1$ for the model to be viable, and $beta_{PN,0}>1$ (but very close to 1) if the model has a significantly phantom DE today. However, prospects to establish the phantom behaviour of DE are much better with cosmological data than with Solar System experiments. Earlier obtained results for a $Lambda$-dominated universe with the vanishing scalar field potential are extended to a more general DE equation of state confirming that the cosmological evolution of these models rule them out. Models of currently fantom DE which are viable for small $z$ can be easily constructed with a constant potential; however, they generically become singular at some higher $z$. With a growing potential, viable models exist up to an arbitrary high redshift." @default.
• W3100252661 created "2020-11-23" @default.
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• W3100252661 date "2006-09-29" @default.
• W3100252661 modified "2023-10-01" @default.
• W3100252661 title "Scalar–tensor models of normal and phantom dark energy" @default.
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• W3100252661 doi "https://doi.org/10.1088/1475-7516/2006/09/016" @default.
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