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Proper Elements, Families, and Belt Boundaries

Published online by Cambridge University Press:  12 April 2016

J.G. Williams
J.G. Williams*
Affiliation:
Jet Propulsion Laboratory

Extract

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Families of asteroids were first found by Hirayama (1918, 1923, 1928). More recently Brouwer (1951) and Arnold (1969) have extended greatly the number of families known from the cataloged asteroids. The Palomar-Leiden survey (PLS) (van Houten et al., 1970), which mainly covered very faint, uncataloged objects, found several more families.

Except for the work of Hirayama (1918), which used osculating elements, all of the above studies looked for clusterings of the semimajor axis a, the proper eccentricities é, and proper inclinations í. The calculation of proper elements involves using a theory of secular perturbations to remove the long-period, large-amplitude disturbances of the major planets. The theory used Up to now (Brouwer and van Woerkom, 1950; Brouwer and Clemence, 1961) involved a low-order expansion in the eccentricities and inclinations. There is now a theory available (Williams, 1969) that will accurately handle much higher eccentricities and inclinations than before.

Type
Part I-Observations
Information
International Astronomical Union Colloquium , Volume 12: Physical Studies of Minor Planets , 1971 , pp. 177 - 181
Copyright
Copyright © NASA 1971

References

Arnold, J.R. 1969, Asteroid Families and Jet Streams. Astron. J. 74, 1235–1242.Google Scholar
Brouwer, D. 1951, Secular Variations of the Orbital Elements of Minor Planets. Astron. J. 56, 9–32.CrossRefGoogle Scholar
Brouwer, D., and Clemence, G.M. 1961, Secular Perturbations. Methods of Celestial Mechanics, ch. 16, pp. 507–529. Academic Press, Inc. New York.Google Scholar
Brouwer, D., and van Woerkom, A.J.J. 1950, The Secular Variations of the Orbital Elements of the Principal Planets. Astron. Papers Amer. Ephemeris, vol. 13, pt. 2, pp. 85–107.Google Scholar
Hirayama, K. 1918, Groups of Asteroids Probably of Common Origin. Astron. J. 31, 185–188.CrossRefGoogle Scholar
Hirayama, K. 1923, Families of Asteroids. Jap. J. Astron. Geophys. 1, 55–105.Google Scholar
Hirayama, K. 1928, Families of Asteroids. (Second Paper.) Jap. J. Astron. Geophys. 5, 137–162.Google Scholar
Houten, C.J. van, Houten-Groeneveld, I. van, Herget, P., and Gehrels, T. 1970, Palomar-Leiden Survey of Faint Minor Planets. Astron. Astrophys. Suppl. Ser. 2(5), 339–448.Google Scholar
Öpik, E.J. 1963, The Stray Bodies in the Solar System. Pt. 1. Survival of Cometary Nuclei and the Asteroids. Advances in Astronomy and Astrophysics, vol. 2, pp. 219–262. Academic Press, Inc. New York.Google Scholar
Williams, J.G. 1969, Secular Perturbations in the Solar System, pp. 1–270. Ph. D. Dissertation, UCLA.Google Scholar