Dark matter versus modifications of the gravitational inverse-square law: results from planetary motion in the Solar system
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Dark matter or modifications of the Newtonian inverse-square law in the Solar system are studied with accurate planetary astrometric data. From extraperihelion precession and possible changes in the third Kepler’s law, we get an upper limit on the local dark matter density, ρDM 3 × 10 −16 kg m −3 at the 2σ confidence level. Variations in the 1/r 2 behaviour are considered in the form of either a possible Yukawa-like interaction or a modification of gravity of Milgrom’s modified Newtonian dynamics (MOND) type. Up to scales of 10 11 m, scale-dependent deviations in the gravitational acceleration are really small. We examined the MOND interpolating function μ in the regime of strong gravity. Gradually varying μ suggested by fits of rotation curves are excluded, whereas the standard form μ(x) = x/(1 + x 2 ) 1/2 is still compatible with data. In combination with constraints from galactic rotation curves and theoretical considerations on the external field effect, the absence of any significant deviation from inverse square attraction in the Solar system makes the range of acceptable interpolating functions significantly narrow. Future radio ranging observations of outer planets with an accuracy of few tenths of a metre could either give positive evidence of dark matter or disprove modifications of gravity.
Subfields: Astronomy and Astrophysics, Oceanography
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Citations in the corpus
- Relativistic effects and dark matter in the Solar system from observations of planets and spacecraft (2013, background): “…detect the possible influence of dark matter on the motion of objects in the solar system have already been made (Nordtvedt, Mueller & Soffel, 1995; Anderson et al., 1989; Anderson et al., 1995; Sereno & Jetzer, 2006; Khriplovich & Pitjeva, 2006; Khriplovich, 2007; Frere, Ling & Vertongen, 2008).”
- Effect of Sun and Planet-Bound Dark Matter on Planet and Satellite Dynamics in the Solar System (2010, background): “Several studies have been dedicated to placing bounds on the local distribution of DM in our solar system from orbital motions of natural major and minor bodies and artificial probes [20, 24, 25, 26, 27, 28, 29, 30, 31, 32, 33, 34, 35, 20, 36, 37]; actually, the upper bound of eq.”
- Modified Newtonian Dynamics (MOND): Observational Phenomenology and Relativistic Extensions (2011, methodology): “In units of a0, the amplitude of the anomalous acceleration is given by x[1−μ(x)], which can be constrained from the motion of the inner planets, typically their perihelion precession and the (non)-variation of Kepler’s constant [294, 391, 418].”
- Quasi-linear formulation of MOND (2009, result): “This, however, is in conflict with solar system constraints (Milgrom 1983, 2009a, Sereno & Jetzer 2006); this would thus rule out the case α+ β = 1.6 6This finding is of the same kind arrived at by Zhao and Famaey (2006) in regard to certain versions of TeVeS.”