Relativistic stars in f(R) and scalar-tensor theories

Details Relativistic stars in f(R) and scalar-tensor theories Relativistic stars in f(R) and scalar-tensor theories

2009-11-06

arxiv.org/abs/0911.1297v3

Phys.Rev.D81:124051,2010

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

20 pages, 10 Figs, revtex4; v2. minor corrections and changes; v3: a few changes, matches published version

Scientific paper

10.1103/PhysRevD.81.124051

We study relativistic stars in the context of scalar tensor theories of gravity that try to account for the observed cosmic acceleration and satisfy the local gravity constraints via the chameleon mechanism. More specifically, we consider two types of models: scalar tensor theories with an inverse power law potential and f(R) theories. Using a relaxation algorithm, we construct numerically static relativistic stars, both for constant energy density configurations and for a polytropic equation of state. We can reach a gravitational potential up to $\Phi\sim 0.3$ at the surface of the star, even in f(R) theories with an "unprotected" curvature singularity. However, we find static configurations only if the pressure does not exceed one third of the energy density, except possibly in a limited region of the star (otherwise, one expects tachyonic instabilities to develop). This constraint is satisfied by realistic equations of state for neutron stars.

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