Quantum vacuum effects as generalized f(R) gravity. Application to stars

Abstract

It is assumed that, for weak spacetime curvature, the main gravitational effect of the quantum vacuum stress-energy corresponds to adding two terms to the Einstein-Hilbert action, proportional to the square of the curvature scalar and to the contraction of two Ricci tensors, respectively. It is shown that compatibility with terrestrial and solar systems observaction implies that the square roorts of the coefficients of these terms should be either a few millimeters or a few hundred meters. It is shown that the vacuum contribution increase the stability of white dwarfs.

GEneralizes and improves previous version

References in corpus (6)

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Cited by in corpus (13)

• Structure of neutron stars in R-squared gravity
• On Wormhole Throats in $f(R)$ Gravity Theory
• Isotropic and Anisotropic Bouncing Cosmologies in Palatini Gravity
• Modified gravity with logarithmic curvature corrections and the structure of relativistic stars
• The most general fourth order theory of Gravity at low energy
• Neutron stars in generalized f(R) gravity
• Cosmology with Hu-Sawicki gravity in Palatini Formalism
• Cosmographic constraints on a class of Palatini f(R) gravity
• Future dynamics in f(R) theories
• Dark energy as a curvature of space-time induced by quantum vacuum fluctuations
• Equation of State of Neutron Stars with Junction Conditions in the Starobinsky Model
• Cosmological Consequences of Exponential Gravity in Palatini Formalism
• Self-gravitating systems in Extended Gravity