A numerical solution of the inverse problem in classical celestial mechanics, with application to Mercury's motion

Details A numerical solution of the inverse problem in classical celestial mechanics, with application to Mercury's motion A numerical solution of the inverse problem in classical celestial mechanics, with application to Mercury's motion

2001-05-14

arxiv.org/abs/astro-ph/0105217v2

Meccanica 39 (2004) 17-29

Astronomy and Astrophysics

Astrophysics

v2: PDF, 17 pages including 4 figures, accepted for publication in Meccanica. Discussion improved, title changed, former Sects

Scientific paper

It is attempted to obtain the masses of the celestial bodies, the initial conditions of their motion, and the constant of gravitation, by a global parameter optimization. First, a numerical solution of the N-bodies problem for mass points is described and its high accuracy is verified. The osculating elements are also accurately computed. This solution is implemented in the Gauss iterative algorithm for solving nonlinear least-squares problems. This algorithm is summarized and its efficiency for the inverse problem in celestial mechanics is checked on a 3-bodies problem. Then it is used to assess the accuracy to which a Newtonian calculation may reproduce the DE403 ephemeris, that involves general-relativistic corrections. The parameter optimization allows to reduce the norm and angular differences between the Newtonian calculation and DE403 by a factor 10 (Mercury, Pluto) to 100 (Venus). The maximum angular difference on the heliocentric positions of Mercury is ca. 220" per century before the optimization, and ca. 20" after it. The latter is still far above the observational accuracy. On the other hand, Mercury's longitude of the perihelion is not affected by the optimization: it keeps the linear advance of 43" per century. Key words: Mercury's perihelion. Parameter optimization. Mechanics of point masses.

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