How the orbital period of a test particle is modified by the Dvali-Gabadadze-Porrati gravity?

Abstract

In addition to the pericentre ω, the mean anomaly M and, thus, the mean longitude λ, also the orbital period Pb and the mean motion $n$ of a test particle are modified by the Dvali-Gabadadze-Porrati gravity. While the correction to Pb depends on the mass of the central body and on the geometrical features of the orbital motion around it, the correction to $n$ is independent of them, up to terms of second order in the eccentricity $e$. The latter one amounts to about 2\times 10^-3 arcseconds per century. The present-day accuracy in determining the mean motions of the inner planets of the Solar System from radar ranging and differential Very Long Baseline Interferometry is 10^-2-5\times 10^-3 arcseconds per century, but it should be improved in the near future when the data from the spacecraft to Mercury and Venus will be available.

LaTex, 7 pages, 13 references, no tables, no figures. Section 2.3 added. To appear in JCAP

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