Hostname: page-component-cd9895bd7-gvvz8 Total loading time: 0 Render date: 2024-12-28T20:20:23.908Z Has data issue: false hasContentIssue false
  • English
  • Français

A Composite Catalogue of Asteroid Proper Elements

Published online by Cambridge University Press:  19 July 2016

Andrea Milani ,
Edward Bowell ,
Zoran Knežević ,
Anne Lemaitre ,
Alessandro Morbidelli  and
Karri Muinonen
Andrea Milani
Affiliation:
Dipartimento di Matematica, Via Buonarroti 2, I-56127 Pisa, Italia E-mail milani@dm.unipi.it
Edward Bowell
Affiliation:
Lowell Observatory, 1400 W. Mars Hill Road, Flagstaff AZ 86001, USA E-mail elgb@lowell.edu
Zoran Knežević
Affiliation:
Astronomska opservatorija, Volgina 7, 11050 Beograd, Yugoslavia
Anne Lemaitre
Affiliation:
Dép. Mathématique, FUNDP, Rempart de la Vierge 8, B-5000 Namur, Belgium E-mail alemaitr@math.fundp.ac.be
Alessandro Morbidelli
Affiliation:
Observatoire de la Côte d'Azur, BP 229, 06304 Nice Cedex 04, France E-mail morby@rameau.obs-nice.fr
Karri Muinonen
Affiliation:
Observatorio, PL 14, 00014 Helsingin yliopisto, Suomi-Finland E-mail karri@ceres.helsinki.fi

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.

We have assembled the asteroid proper elements computed by different authors, using different methods, and for different regions of the asteroid belt. Asteroids on planet crossing orbits are not yet included. The use of very different algorithms is dictated by the dynamics of the different regions. For the asteroids of the main belt, having semimajor axes between 2.1 and 3.8 AU, and with proper eccentricity and sine of inclination less than 0.3, proper elements are computed by a fully analytical iterative theory developed by Milani and Knežević (1990,1992,1994; hereafter M&K). For high inclination and/or eccentricity main-belt asteroids, having 1.8 < a < 3.8 AU and either e or sin I larger than 0.24, proper elements are computed by a semianalytical theory developed by Lemaitre and Morbidelli (1994; hereafter L&M). For Trojans, proper elements are computed by a synthetic theory (that is, from the output of a numerical integration for a few Myr) by Milani (1993). For the Hilda asteroids in the 3: 2 resonance, proper elements have been computed by a synthetic theory by Schubart (1982, 1991). For a discussion of the state of the art in the computation of proper elements, see Knežević and Milani, this volume; for Trojans, see Milani, this volume; for some other cases (e.g. proper elements for resonant asteroids), see Froeschlé and Morbidelli, this volume. When and if new proper elements will be available for other asteroids, they will be added to the public domain file, together with updates and upgrades of the existing catalogues.

Type
Data Bases
Information
Symposium - International Astronomical Union , Volume 160: Asteroids, Comets, Meteors 1993 , 1994 , pp. 467 - 470
Copyright
Copyright © Kluwer 1994 

References

Knežević, Z. 1988. “Asteroid mean orbital elements”. Bull. Astron. Obs. Belgrade 139, 1–6.Google Scholar
Lemaitre, A., and Morbidelli, A. 1994. “Calculation of proper elements for high inclined asteroidal orbits”. Celest. Mech., in press.Google Scholar
Milani, A. 1993. “The Trojan asteroid belt: proper elements, stability, chaos and families”. Celest. Mech., 57, 59–94.CrossRefGoogle Scholar
Milani, A., and Knežević, Z. 1990. “Secular perturbation theory and computation of asteroid proper elements”. Celestial Mechanics 49, 347–411.Google Scholar
Milani, A., and Knežević, Z. 1992. “Asteroid proper elements and secular resonances”. Icarus, 98, 211–232.CrossRefGoogle Scholar
Milani, A., and Knežević, Z. 1994. “Asteroid proper elements and the dynamical structure of the asteroid main belt”. Icarus, in press.Google Scholar
Milani, A., Farinella, P., and Knežević, Z. 1992. “On the search for asteroid families”. In Interrelations between physics and dynamics for minor bodies in the solar system (Benest, D., Froeschléi, C., Eds.), 85–132, Editions Frontières, Gif–sur–Yvette.Google Scholar
Muinonen, K., and Bowell, E. 1993. “Asteroid orbit determination using Bayesian probabilities”. Icarus 104, 255–279.CrossRefGoogle Scholar
Muinonen, K., Bowell, E. and Wasserman, L.H. 1994. “Orbital uncertainities of single–opposition asteroids.” Planet. Space Sci., in press.CrossRefGoogle Scholar
Schubart, J. 1982. “Three characteristic parameters of orbits of Hilda type asteroids”. Astron. Astrophys. 114, 200–204.Google Scholar
Schubart, J. 1991. “Additional results on orbits of Hilda type asteroids”. Astron. Astrophys. 241, 297–302.Google Scholar
Zappalà, V., Cellino, A., Farinella, P., and Knežević, Z. 1990. “Asteroid families I: identification by hierarchical clustering and reliability assessment”. Astron. J. 100, 2030–2046.Google Scholar