A modified model of non-locally corrected gravity: Cosmology and the Newtonian limit

Abstract

A modified form of non-locally corrected theory of gravity is investigated in the context of cosmology and the Newtonian limit. This form of non-local correction to classic Einstein-Hilbert action can be locally represented by a triple-scalar-tensor theory in which one of the scalar degree of freedom is phantom-like and the other two are quintessence-like. We show that there exists a stable de Sitter solution for the cosmological dynamics if a suitable form of potential function $V(\varphi )$ (or equivalently, $f(R)$) is selected. However, no matter what a potential function is selected, there is always an early time repeller solution corresponding to a radiation dominated universe. Besides, the equations for linear scalar perturbations are presented and it is shown that the form of potential function $V(\varphi )$ is stringently constrained by the Solar system test, although the post-Newtonian parameter $\gamma$ is not directly affected by this function.

11 pages, 2 figures; V2:reference added; matched with the published version

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Cited by in corpus (2)

• Acausality in Nonlocal Gravity Theory
• Ghosts in classes of non-local gravity