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Title:
Existence of relativistic stars in f(R) gravity
Authors:
Upadhye, Amol; Hu, Wayne
Affiliation:
AA(Kavli Institute for Cosmological Physics, Enrico Fermi Institute, University of Chicago, Chicago, Illinois 60637, USA), AB(Kavli Institute for Cosmological Physics, Enrico Fermi Institute, University of Chicago, Chicago, Illinois 60637, USA; Department of Astronomy and Astrophysics, University of Chicago, Chicago, Illinois 60637, USA)
Publication:
Physical Review D, vol. 80, Issue 6, id. 064002 (PhRvD Homepage)
Publication Date:
09/2009
Origin:
APS
PACS Keywords:
Modified theories of gravity
Abstract Copyright:
(c) 2009: The American Physical Society
DOI:
10.1103/PhysRevD.80.064002
Bibliographic Code:
2009PhRvD..80f4002U

Abstract

We refute recent claims in the literature that stars with relativistically deep potentials cannot exist in f(R) gravity. Numerical examples of stable stars, including relativistic (GM⋆/r⋆˜0.1), constant density stars, are studied. As a star is made larger, nonlinear “chameleon” effects screen much of the star’s mass, stabilizing gravity at the stellar center. Furthermore, we show that the onset of this chameleon screening is unrelated to strong gravity. At large central pressures P>ρ/3, f(R) gravity, like general relativity, does have a maximum gravitational potential, but at a slightly smaller value: GM⋆/r⋆|max⁡=0.345<4/9 for constant density and one choice of parameters. This difference is associated with negative central curvature R under general relativity not being accessed in the f(R) model, but does not apply to any known astrophysical object.
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