Late time cosmic acceleration from vacuum Brans-Dicke theory in 5D

Abstract

We show that the scalar-vacuum Brans-Dicke equations in 5D are equivalent to Brans-Dicke theory in 4D with a self interacting potential and an effective matter field. The cosmological implication, in the context of FRW models, is that the observed accelerated expansion of the universe comes naturally from the condition that the scalar field is not a ghost, i.e., $\omega >-3/2$. We find an effective matter-dominated 4D universe which shows accelerated expansion if $-3/2<\omega <-1$. We study the question of whether accelerated expansion can be made compatible with large values of $\omega$, within the framework of a 5D scalar-vacuum Brans-Dicke theory with variable, instead of constant, parameter $\omega$. In this framework, and based on a general class of solutions of the field equations, we demonstrate that accelerated expansion is incompatible with large values of $\omega$.

In V2 the summary section is expanded. To be published in Classical and Quantum Gravity.

References in corpus (1)

• Brans-Dicke Scalar Field as a Chameleon

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