The interior spacetimes of stars in Palatini f(R) gravity

Abstract

We study the interior spacetimes of stars in the Palatini formalism of f(R) gravity and derive a generalized Tolman-Oppenheimer-Volkoff and mass equation for a static, spherically symmetric star. We show that matching the interior solution with the exterior Schwarzschild-De Sitter solution in general gives a relation between the gravitational mass and the density profile of a star, which is different from the one in General Relativity. These modifications become neglible in models for which $\delta F(R)\equiv \partial f/\partial R-1$ is a decreasing function of R however. As a result, both Solar System constraints and stellar dynamics are perfectly consistent with $f(R)=R-{\mu }^4/R$.

Published version, 6 pages, 1 figure

References in corpus (2)

• Solar System tests DO rule out 1/R gravity
• Constraints on f(R) Cosmology in the Palatini Formalism

Cited by in corpus (7)

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• Viable Palatini-f(R) cosmologies with generalized dark matter
• Re-examination of Polytropic Spheres in Palatini f(R) Gravity
• On the stability of spherically symmetric spacetimes in metric f(R) gravity
• Maximal symmetry and metric-affine f(R) gravity