2010/04/12 by Joachim Näf, Philippe Jetzer · 3 citations
Physics and Astronomy · #Black Holes and Theoretical Physics #Cosmology and Gravitation Theories #Relativity and Gravitational Theory #astro-ph.EP #gr-qc
paper · pdf · doi:10.1103/physrevd.81.104003
published as Phys.Rev.D81:104003,2010 · 11 pages, accepted for publication in Physical Review D
arxiv created 2010/04/12 · openalex publication_date 2010/05/04 · arxiv updated 2010/05/25 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/29
We derive for applications to isolated systems---on the scale of the Solar System---the first relativistic terms in the 1/c expansion of the space time metric g_\ensuremathμ\ensuremathν for metric f(R) gravity theories, where f is assumed to be analytic at R=0. For our purpose it suffices to take into account up to quadratic terms in the expansion of f(R), thus we can approximate f(R)=R+aR2 with a positive dimensional parameter a. In the nonrelativistic limit, we get an additional Yukawa correction with coupling strength G/3 and Compton wave length √(6a) to the Newtonian potential, which is a known result in the literature. As an application, we derive to the same order the correction to the geodetic precession of a gyroscope in a gravitational field and the precession of binary pulsars. The result of the Gravity Probe B experiment yields the limit a\ensuremath\lesssim5\ifmmode×\else\texttimes\fi1011 m2, whereas for the pulsar B in the PSR J0737-3039 system we get a bound which is about 104 times larger. On the other hand the E"ot-Wash experiment provides the best laboratory bound a\ensuremath\lesssim10^\ensuremath-10 m2. Although the former bounds from geodesic precession are much larger than the laboratory ones, they are still meaningful in the case some type of chameleon effect is present and thus the effective values could be different at different length scales.