Hostname: page-component-77c89778f8-swr86 Total loading time: 0 Render date: 2024-07-21T20:19:43.226Z Has data issue: false hasContentIssue false
  • English
  • Français

Higher Order and Iterative Theories to Compute Asteroid Mean Elements

Published online by Cambridge University Press:  12 April 2016

Z. Knežević  and
A. Milani
Z. Knežević
Affiliation:
Astronomical Observatory, Volgina 7, 11160 Belgrade 74, YugoslaviaE-mail:zoran@aob.bg.ac.yu
A. Milani
Affiliation:
Department of Mathematics, Via Buonarroti 2, 56127 Pisa, ItalyE-mail:milani@dm.unipi.it

Extract

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.

Mean orbital elements are obtained from their instantaneous, osculating counterparts by removal of the short periodic perturbations. They can be computed by means of different theories, analytical or numerical, depending on the problem and accuracy required. The most advanced contemporary analytical theory (Knežević 1988) accounts only for the perturbing effects due to Jupiter and Saturn, to the first order in their masses and to degree four in eccentricity and inclination. Nevertheless, the mean elements obtained by means of this theory are of satisfactory accuracy for majority of the asteroids in the main belt (Knežević et al. 1988), for the purpose of producing large catalogues of mean and proper elements, to identify asteroid families, to assess their age, to study the dynamical structure of the asteroid belt and chaotic phenomena of diffusion over very long time spans. In the vicinity of the main mean motion resonances, however, especially 2:1 mean motion resonance with Jupiter, these mean elements are of somewhat degraded accuracy.

Type
Extended Abstracts
Information
International Astronomical Union Colloquium , Volume 172: Impact of Modern Dynamics in Astronomy , 1999 , pp. 359 - 360
Copyright
Copyright © Kluwer 1999

References

Breiter, S., 1997a, Celest. Mech. Dyn. Astron., 65, 345–354.Google Scholar
Breiter, S., 1997b, Celest. Mech. Dyn. Astron., 67, 237–249.Google Scholar
Knežević, Z., 1988, Bull. Astron. Obs. Belgrade, 139, 1–6.Google Scholar
Knežević, Z., Carpino, M., Farinella, P., Froeschlé, Ch., Froeschlé, CI., Gönczi, R., Jovanović, B., Paolicchi, P., and Zappalà, V., 1988, Astron. Astrophys., 192, 360–369.Google Scholar
Milani, A., 1988, In: Long-term Dynamical Behaviour of Natural and Artificial N-Body Systems (Roy, A.E., Ed.), Kluwer Acad. Publ., pp. 73–108.CrossRefGoogle Scholar
Milani, A., and Knežević, Z., 1990, Celest. Mech. Dyn. Astron., 49, 247–411.Google Scholar
Milani, A., and Knežević, Z., 1994, Icarus, 107, 219–254.CrossRefGoogle Scholar
Milani, A., and Knežević, Z., 1998, Celest. Mech. Dyn. Astron., in press.Google Scholar