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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 generalization of Einstein's general relativity (GR), the f( R, T) gravity replace the gravitational Lagrangian of GR with an arbitrary function of the Ricci scalar R and of the trace of the stress-energy tensor T. It can induce an extra acceleration a in the dynamics of massive test particles due to the physical coupling between matter and geometry. In this work, we confront this extra acceleration with planetary motions in the solar system. Using the supplementary advances in the perihelia provided by current INPOP10a and EPM2011 ephemerides, we obtain new upper limits on a when the uncertainty of the Sun's quadrupole moment and the Lense-Thirring effect due to the Sun's angular momentum are properly taken into account. These two factors were mostly absent in previous works dealing with a. We find that INPOP10a yields the upper limit as a=(−0.04±4.81)×10 m s and EPM2011 gives a=(0.06±1.58)×10 m s . Both of them are improved at least by about 10 times than previous results obtained in the solar system and they are smaller than the results given by fitting rotation curves of galaxies by about 4 orders of magnitude. This discrepancy of a on these scales seems to imply that its effects might be screened 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]