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• W2136868863 abstract "$f(R)$ gravity is one of the simplest theories of modified gravity to explain the accelerated cosmic expansion. Although it is usually assumed that the quasi-Newtonian approach (a combination of the quasistatic approximation and sub-Hubble limit) for cosmic perturbations is good enough to describe the evolution of large scale structure in $f(R)$ models, some studies have suggested that this method is not valid for all $f(R)$ models. Here, we show that in the matter-dominated era, the pressure and shear equations alone, which can be recast into four first-order equations to solve for cosmological perturbations exactly, are sufficient to solve for the Newtonian potential, $mathrm{ensuremath{Psi}}$, and the curvature potential, $mathrm{ensuremath{Phi}}$. Based on these two equations, we are able to clarify how the exact linear perturbations fit into different limits. We find that the Compton length controls the quasistatic behaviors in $f(R)$ gravity. In addition, regardless the validity of quasistatic approximation, a strong version of the sub-Hubble limit alone is sufficient to reduce the exact linear perturbations in any viable $f(R)$ gravity to second order. Our findings disagree with some previous studies where we find little difference between our exact and quasi-Newtonian solutions even up to $k=10{c}^{ensuremath{-}1}{mathcal{H}}_{0}$." @default.
• W2136868863 created "2016-06-24" @default.
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• W2136868863 date "2015-11-18" @default.
• W2136868863 modified "2023-10-04" @default.
• W2136868863 title "Cosmological perturbations and quasistatic assumption inf(R)theories" @default.
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• W2136868863 doi "https://doi.org/10.1103/physrevd.92.103514" @default.
• W2136868863 hasPublicationYear "2015" @default.
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