Solar system planetary orbital motions and dark matter
By Lorenzo Iorio. 2006
36 citations recorded by the source corpus.
In this paper we explicitly work out the effects that a spherically symmetric distribution of dark matter with constant density would induce on the Keplerian orbital elements of the Solar System planets and compare them with the latest results in planetary orbit determination from the EPM2004 ephemerides. It turns out that the longitudes of perihelia ϖ and the mean longitudes λ are affected by secular precessions. The resulting upper bounds on dark matter density, obtained from the EPM2004 formal errors in the determined mean longitude shifts over 90 years, lie in the range 10−19–10−20 g cm−3 with a peak of 10−22 g cm−3 for Mars. Suitable combinations of the planetary mean longitudes and perihelia, which cancel out the aliasing impact of some of the unmodelled or mismodelled forces of the dynamical models of EPM2004, yield a global upper bound of 7 × 10−20 and 4 × 10−19 g cm−3, respectively.
Subfields: Astronomy and Astrophysics
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Citations in the corpus
- 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.”
- Dark matter versus modifications of the gravitational inverse-square law: results from planetary motion in the Solar system (2006, background): “In fact, effects on orbits of inner and outer planets would be large enough to have been detected given the present levels of accuracy (Anderson et al. 2002; Iorio 2006b; Sanders 2006).”