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 gμν 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≲5×1011m2, 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 Eöt-Wash experiment provides the best laboratory bound a≲10-10m2. 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.

Näf, J; Jetzer, P (2010). *On the 1/c expansion of f(R) gravity.* Physical Review D, 81(10):104003-8pp.

## Abstract

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 gμν 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≲5×1011m2, 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 Eöt-Wash experiment provides the best laboratory bound a≲10-10m2. 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.

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## Additional indexing

Item Type: | Journal Article, refereed, original work |
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Communities & Collections: | 07 Faculty of Science > Institute for Computational Science |

Dewey Decimal Classification: | 530 Physics |

Language: | English |

Date: | May 2010 |

Deposited On: | 01 Mar 2011 10:04 |

Last Modified: | 05 Apr 2016 14:33 |

Publisher: | American Physical Society |

ISSN: | 1550-2368 |

Publisher DOI: | https://doi.org/10.1103/PhysRevD.81.104003 |

Related URLs: | http://arxiv.org/abs/1004.2014 |

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