A new approach to cosmological perturbations in f(R) models

Abstract

We propose an analytic procedure that allows to determine quantitatively the deviation in the behavior of cosmological perturbations between a given f(R) modified gravity model and a LCDM reference model. Our method allows to study structure formation in these models from the largest scales, of the order of the Hubble horizon, down to scales deeply inside the Hubble radius, without employing the so-called "quasi-static" approximation. Although we restrict our analysis here to linear perturbations, our technique is completely general and can be extended to any perturbative order.

21 pages, 2 figures; Revised version according to reviewer's suggestions; Typos corrected; Added References

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• Relativistic scalar fields and the quasi-static approximation in theories of modified gravity
• Probing Modified Gravity Theories with ISW and CMB Lensing
• Cosmological bounces in spatially flat FRW spacetimes in metric f(R) gravity
• Do cosmological data rule out $f(\mathcal{R})$ with $w\ne -1$?
• Relation between the Turnaround radius and virial mass in $f(R)$ model
• Future CMB ISW-Lensing bispectrum constraints on modified gravity in the Parameterized Post-Friedmann formalism
• Withholding Potentials, Absence of Ghosts and Relationship between Minimal Dilatonic Gravity and f(R) Theories
• Scalar-Induced Gravitational Waves in Modified Gravity
• Early universe cosmological solutions in exponential gravity
• Scalar-Induced Gravitational Waves in Palatini $f(R)$ Gravity