Hostname: page-component-77c89778f8-gq7q9 Total loading time: 0 Render date: 2024-07-22T11:40:16.695Z Has data issue: false hasContentIssue false
  • English
  • Français

The precision of modern theories of Galilean satellites as derived with their comparison with photographic observations made with the 26″ refractor at Pulkovo Observatory

Published online by Cambridge University Press:  04 August 2017

T. P. Kisseleva ,
N. I. Glebova  and
A. G. Malkova
T. P. Kisseleva
Affiliation:
Main Astronomical Observatory, 196140 Leningrad, U.S.S.R.
N. I. Glebova
Affiliation:
Institute of Theoretical Astronomy, 191187 Leningrad, U.S.S.R.
A. G. Malkova
Affiliation:
Institute of Theoretical Astronomy, 191187 Leningrad, U.S.S.R.

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The regular photographic observations of Galilean satellites has been made with 26″ refractor at Pulkovo since 1975. The relative positions of satellites are obtained by means of “scaletrail” technique. During 1975–1979 over 600 observations of Galilean satellites were carried out. The observed positions were compared with the ephemeris based on Sampson's and Lieske's E-1 theories, the corresponding computations being made at the Institute for Theoretical Astronomy. The standard deviations of one observed relative position “Satellite minus Jupiter” don't exceed ±0″.10. The comparison of Sampson's theory with observations showed some systematic error which can be considered as an error in longitude of about 1 min. Lieske's theory E-1 showed a better agreement with the observations, the absolute deviations not exceeding 0″.3.

A construction of highly precision theories of motion of planet's satellites and of Galilean satellites, in particular, demands appropriately accurate observations (the error not exceeding 0″.10). At present such observations of satellites can be obtained with the help of long-foci telescopes (focal length of about 10 m), using rigorous technique of astrometric reduction.

Type
Motions of Natural Bodies in the Solar System
Information
Symposium - International Astronomical Union , Volume 114: Relativity in Celestial Mechanics and Astrometry , 1986 , pp. 129 - 134
Copyright
Copyright © Reidel 1986 

References

Kisselev, A.A., 1971. Izv. Gl. Astr. Obs. Pulkovo N187, pp. 49–57.Google Scholar
Kisselev, A.A., 1964. Izv. Gl. Astr. Obs. Pulkovo N174, pp. 120–125.Google Scholar
Kisseleva, T.P., 1985. Izv. Gl. Astr. Obs. Pulkovo N201, pp. 71–76.Google Scholar
Kisselev, A.A., and Bystrov, N.F., 1976. Izv. Gl. Astr. Obs. Pulkovo N194, pp. 139–148.Google Scholar
Sampson, R.H., 1910. Tables of the four Great Satellites of Jupiter, London.CrossRefGoogle Scholar
Andoyer, H., 1915. Bull. Astron. XXXII, pp. 177–220.CrossRefGoogle Scholar
Lieske, J.H., 1977. Astron. and Astrophys. 56, pp. 333–352.Google Scholar
Lieske, J.H., 1978. Astron. and Astrophys. 65, pp. 83–92.Google Scholar