Solar System planetary orbital motions and dark matter
arXiv:gr-qc/0602095 · doi:10.1088/1475-7516/2006/05/002
Abstract
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 and the mean longitudes 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 g cm^-3 and 4 10^-19 g cm^-3, respectively.
Latex, 8 pages, 2 tables, no figures, 8 references. Revised version with improved analysis
References in corpus (4)
- WIMP diffusion in the solar system including solar depletion and its effect on Earth capture rates
- Improved bounds on non-luminous matter in solar orbit
- Upper limits on density of dark matter in Solar system
- Is it possible to measure the Lense-Thirring effect on the orbits of the planets in the gravitational field of the Sun?
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