Determination of the masses of Saturn and Uranus from an analysis of the motion of the minor planets (944) Hidalgo and (2060) Chiron. (German Title: Ein Beitrag zur Massenbestimmung der Planeten Saturn und Uranus aufgrund einer Analyse der Bewegung der

Details Determination of the masses of Saturn and Uranus from an analysis of the motion of the minor planets (944) Hidalgo and (2060) Chiron. (German Title: Ein Beitrag zur Massenbestimmung der Planeten Saturn und Uranus aufgrund einer Analyse der Bewegung der Determination of the masses of Saturn and Uranus from an analysis of the motion of the minor planets (944) Hidalgo and (2060) Chiron. (German Title: Ein Beitrag zur Massenbestimmung der Planeten Saturn und Uranus aufgrund einer Analyse der Bewegung der

Mar 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983a%26a...119...95l&link_type=abstract

Astronomy and Astrophysics, vol. 119, no. 1, Mar. 1983, p. 95-100. In German.

Astronomy and Astrophysics

Astrophysics

5

Gravitational Effects, Planetary Mass, Saturn (Planet), Uranus (Planet), Chiron, Errors, Perturbation, Planetary Orbits, Planets, Saturn, Uranus, Mass, Motion, Asteroids, Hidalgo 944 Asteroid, Chiron 2060 Asteroid, Calculations, Perturbations, Observations, Data

Scientific paper

Values for the masses of Saturn and Uranus are computed by their perturbations on the motion of (944) Hidalgo and (2060) Chiron. From 210 observations of Hidalgo, distributed over 12 oppositions 1921 to 1978 we find masses of (1:3498.03 ± 0.07) Msun for Saturn and (1:230651 ± 115) Msun for Uranus. From 33 observations over 10 oppositions 1895-1981 of Chiron we obtain (1:230901 253) solar masses for Uranus (including satellites; errors are mean errors).
Because the influence of errors on fundamental data such as the adopted masses of other planets is not small, we suggest to solve the normal equations under small variation of these data and publish the derivatives in addition to the values of the results. By collecting and solving such equations from different authors, one may probably obtain a much more consistent system of planetary masses than by a simple averaging of the individual results.

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