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By making use of the supplementary advances of the perihelia provided by INPOP10a and INPOP15a (France) and EPM2011 (Russia) ephemerides, we obtain improved Solar System bounds on the cosmologically viable $f(\mathcal{G})$ gravity, where $f$ is an arbitrary function of the Gauss-Bonnet invariant $\mathcal{G}$ . When we estimate new bounds on its model parameters, we consider the Lense-Thirring effect caused by the Sun's angular momentum and the uncertainty of the Sun's quadrupole moment, neither of which were included in related works before. The bounds we obtain in the present work are tighter than the previous ones by at least 5 orders of magnitude. [ABSTRACT FROM AUTHOR]

A recent model of nonlocal gravity is tested by the dynamics of the Solar System. This theory of gravity goes beyond the hypothesis of locality and includes the past history of an observer into measurements. Using the supplementary advances of the perihelia provided by INPOP10a (IMCCE, France) and EPM2011 (IAA RAS, Russia) ephemerides, we obtain the bounds on its parameters: α and λ 0 . In this investigation, we take the Lense–Thirring effect due to the Sun’s angular momentum and the uncertainty of the Sun’s quadrupole moment into account. These two factors were usually absent in previous works. We find that INPOP10a yields the Solar System’s bounds as α = ( − 0.6 ± 12 ) × 1 0 − 12 and λ 0 = ( 0.2 ± 2.1 ) × 10 5 kpc, while EPM2011 gives α = ( 0.3 ± 3.2 ) × 1 0 − 12 and λ 0 = ( − 0.4 ± 1.7 ) × 10 5 kpc. The bound of α is considerably smaller than the result based on the rotation curves of spiral galaxies and the bound of λ 0 is much larger than the one based on the rotation curves by at least 5 orders of magnitude. It makes the nonlocal gravity much weaker in the scale of the Solar System than it in the scale of galaxies, implying that a screening mechanism is required to suppress the nonlocal gravity in high density regions. [ABSTRACT FROM AUTHOR]

As a power class of generalization of Einstein’s general relativity, the R 1 + δ gravity is confronted with planetary motions in the solar system. Using the supplementary advances in the perihelia provided by current INPOP10a (IMCCE, France) and EPM2011 (IAA RAS, Russia) ephemerides, we obtain new upper limits on δ in the solar system when the Lense–Thirring effect due to the Sun’s angular momentum and the uncertainty of the Sun’s quadrupole moment are properly taken into account. These two factors were mostly absent in previous works dealing with δ . We find that INPOP10a yields the upper limit as δ = ( 0.6 ± 4.4 ) × 10 - 24 and EPM2011 gives δ = ( 7.5 ± 3.4 ) × 10 - 24 . Both of them are improved by about 5 orders of magnitude than previous result. [ABSTRACT FROM AUTHOR]

Using the supplementary advances of the perihelia provided by INPOP10a (IMCCE, France) and EPM2011 (IAA RAS, Russia) ephemerides, we obtain preliminary limits on a logarithmic correction to the Newtonian gravitational potential in the solar system. This kind of correction may originate from fundamental frameworks, like string theories or effective models of gravity due to quantum effects and the non-local gravity scheme. We estimate upper limit of Tohline-Kuhn-Kruglyak parameter λ and lower bound of Fabris-Campos parameter α, which parametrize the correction and connect each other by αλ=−1. In our estimation, we take the Lense-Thirring effect due to the Sun's angular momentum and the uncertainty of the Sun's quadrupole moment into account. These two factors were usually absent in previous works. We find that INPOP10a yields the upper limit as α=−(0.66±5.82)×10 kpc [or the lower limit as λ=(0.15±8.76)×10 kpc] while EPM2011 gives α=(0.52±1.74)×10 kpc [or the lower limit as λ=−(0.19±3.29)×10 kpc]. The limits of | λ| are greater than the result based on the rotation curves of spiral galaxies by about 3 orders of magnitude, indicating its effects might be screened in high density regions. [ABSTRACT FROM AUTHOR]

Ground-based and space-borne observatories studying exoplanetary transits now and in the future will considerably increase the number of known exoplanets and the precision of the measured times of transit minima. Variations in the transit times can not only be used to infer the presence of additional planets, but might also provide opportunities for testing new physics in the places beyond the Solar system. In this work, we take deviation from the inverse-square law of gravity as an example, focus on the fifth-force-like Yukawa-type correction to the Newtonian gravitational force which parameterizes this deviation, investigate its effects on the secular transit timing variations and analyse their observability in exoplanetary systems. It is found that the most optimistic values of Yukawa-type secular transit timing variations are at the level of ∼0.1 s per year. Those values unfortunately appear only in rarely unique cases and, most importantly, they are still at least two orders of magnitude below the current capabilities of observations. Such a deviation from the inverse-square law of gravity is likely too small to detect for the foreseeable future. Meanwhile, systematic uncertainties, such as the presence of additional and unknown planets, will likely be exceptionally difficult to remove from a signal that should be seen. [ABSTRACT FROM AUTHOR]

The Yukawa correction to the Newtonian gravitational force is accepted as a parametrization of deviations from the inverse-square law of gravity which might be caused by new physics beyond the standard model of particles and the general theory of relativity. We investigate these effects on the clock onboard a drag-free satellite: dynamics of the satellite and influence on the time transfer link. We find that the Yukawa signal in the time transfer is much more difficult to detect with the current state of clocks than those effects on the dynamics, especially the secular change of periastron, by laser ranging in the case of an artificial Earth satellite carrying a frequency standard with an orbit of a = 107 m and e = 0.01. [ABSTRACT FROM AUTHOR]