Solar system planetary motion to third order of the masses
Received 10 March 1998 / Accepted 27 August 1998
We present in this paper a new solution for planetary motion. It consists in developing the perturbations up to the third order of the planetary masses and uses the IERS92 masses set. The relativistic perturbations expressed in isotropic coordinates and the perturbations of the Moon on the inner planets are also included. Effects of asteroids on Earth-Moon barycenter, Mars and Jupiter have been taken into account. We used adjustments to numerical DE403 and DE405 integrations of the Jet Propulsion Laboratory (JPL) to obtain the theory's integration constants.
Key words: celestial mechanics, stellar dynamics ephemerides solar system: general
This article contains no SIMBAD objects.
© European Southern Observatory (ESO) 1999
Online publication: November 26, 1998