Hostname: page-component-848d4c4894-tn8tq Total loading time: 0 Render date: 2024-06-16T21:35:32.400Z Has data issue: false hasContentIssue false
  • English
  • Français

Using Close Encounters of Minor Planets for the Improvement of their Masses

Published online by Cambridge University Press:  12 April 2016

A. López García ,
Yu. D. Medvedev  and
J. A. Moraño Fernández
A. López García
Affiliation:
Astronomical Observatory, Valencia University Valencia, Spain
Yu. D. Medvedev
Affiliation:
Institute of Theoretical Astronomy, Russian Acad, of Sciences St. Petersburg, Russia
J. A. Moraño Fernández
Affiliation:
Department of Astronomy and Astrophycics Valencia, Spain

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 orbits of 6807 numbered minor planets on the time interval 1975–2010 have been integrated. The possibility of determining masses for asteroids with close encounters with each other has been investigated, including several kinds of situations. The importance of the observational time arc, as well as the distribution of observations, for determining the masses are shown. The mass of asteroid (24) Themis from its perturbations on asteroid (2296) Kugultinov, and the mass of (10) Hygiea from its perturbations on (1259) Ógyalla have been determined.

Type
Solar System Dynamics
Information
International Astronomical Union Colloquium , Volume 165: Dynamics and Astrometry of Natural and Artificial Celestial Bodies , 1997 , pp. 199 - 204
Copyright
Copyright © Kluwer 1997

References

Dubyago, A.D.: 1961, The Determination of Orbits, The Macmillan Company, New York.Google Scholar
Everhart, E.: 1985, “An efficient integrator that used Gauss-Radau spacing”, in: Dynamics of Comets: Their Origin and Evolution (Carusi, A. Valsecchi, G.B. eds), Reidel, Dordrecht, 185–202.CrossRefGoogle Scholar
Hilton, J.L., Middour, J., and Seidelmann, P.K.: 1995, “Prospects for determining masses for asteroids”, in: Dynamics, Ephemerides and Astrometry of the Solar System, IAU Symposium 172 (Ferraz-Mello, S., Morando, B., Arlot, J.E., eds), Kluwer, Dordrecht.Google Scholar
Hilton, J.L.: 1996, “The mass of 15 Eunomia”, Abstracts of the International Conference on Asteroids, Comets and Meteors, held in Versailles.Google Scholar
Landgraf, W.: 1992, “A determination of the mass of (704) Interamnia from observations of (993) Moultona”, in: Chaos, Resonance and Collective Dynamical Phenomenon in the Solar System, IAU Symposium 152 (Ferraz-Mello, S. ed.), Kluwer, Dordrecht, 179–182.Google Scholar
Scholl, H., Schmadel, L.D., and Röser, S.: 1987, “The mass of the asteroid (10) Hygiea derived from observations of (820) Academia”, Astron. Astrophys. 170, 311–316.Google Scholar
Schubart, J.: 1975, “The masses of the first two asteroids”, Astron. Astrophys. 39, 147–148.Google Scholar
Schubart, J. and Matson, D.L.: 1979, “Masses and densities of asteroids”, in: Asteroids (Gehreis, T. ed.), Tucson, 84–97.Google Scholar
Standish, E.M. and Hellings, R.W.: 1989, “A determination of the masses of Ceres, Pallas and Vesta from their perturbations upon the orbit of Mars”, Icarus 80, 326–333.CrossRefGoogle Scholar
Viateau, B. and Rapaport, M.: 1995, “The orbit of (2) Pallas”, Astron. Astrophys., Suppl. Ser. 111, 305–310.Google Scholar
Williams, J.G.: 1984, “Determining asteroid masses from perturbation on Mars”, Icarus 57, 1–13.CrossRefGoogle Scholar