Abstract
A simple explanation of some characteristics of the present distribution of number vs. semimajor axis and number vs. eccentricity of the asteroids is obtained in the framework of the restricted three-body problem, choosing suitable initial conditions. We compare the results with the numerical ones by Lecar and Franklin (1973), and we try to explain the depletion of the zone beyond 3.2 A.U. as a possible effect of a primeval collisional process.
Article PDF
Similar content being viewed by others
Avoid common mistakes on your manuscript.
References
Arnold, J. R.: 1965,Astrophys. J. 141, 1536.
Chapman, C. R. and Davis, D. R.: 1975,Science 190, 553.
Dohnanyi, J. S.: 1969,J. Geophys. Res. 74, 2531.
Gaska, S.: 1974, in Y. Kozai (ed.), ‘The Stability of the Solar System and of Small Stellar Systems’IAU Symp. 62, 59–62.
Hartmann, W. K. and Hartmann, A. C.: 1968,Icarus 8, 361.
Lecar, M. and Franklin, F. A.: 1973,Icarus 20, 422.
McAdoo, D. C. and Burns, J. A.: 1973,Icarus 18, 285.
Richter, N.: 1960,Forsch. Fortschr. 34, 66.
Taff, L. G.: 1973,Icarus 20, 21.
Van Houten, C. J., Van Houten-Groeneveld, I., Herget, P. and Gehrels, T.: 1970,Astron. Astrophys. Suppl. 2, 339.
Wetherill, G. W.: 1967,J. Geophys. Res. 72, 2429.
Author information
Authors and Affiliations
Rights and permissions
About this article
Cite this article
Farinella, P., Nobili, A.M. A simple explanation of some characteristics of the asteroidal belt based on the restricted three-body problem. The Moon and the Planets 18, 241–250 (1978). https://doi.org/10.1007/BF00896746
Received:
Issue Date:
DOI: https://doi.org/10.1007/BF00896746