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Steady State Number of the Extinct Comets in High-Inclination Orbits

Published online by Cambridge University Press:  12 April 2016

Tsuko Nakamura
Tsuko Nakamura*
Affiliation:
Dodaira Station, Tokyo Astronomical Observatory, Tokigawa, Hiki-gun, Saitama 355-05 Japan

Abstract

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Steady state number of the short-period(SP) comets captured from nearly parabolic(NP) orbits with 60°≤ i(inclination) ≤ 120° and 0.5≤q (perihelion distance) ≤1.5 AU is calculated. Due to smallness of the q and slowness of the capture process, almost all these SP comets become completely extinct. Combining annual flux of the observed NP comets of high inclination with the capture probability from NP to SP orbits and the ejection rate in SP orbits obtained by Monte Carlo simulations, we find that the steady state number of the extinct SP comets in high-inclination orbits is at least 1-2 hundred. If this number can be considered to correspond to the observed one of Apollo-type objects with i ≥ 60°, it is concluded that only less than a few percent of extinct comets leaves sizable non-volatile cores or shells. The number of asteroid-like bodies deduced from the extinct comets with small perihelion distance and high inclination has less ambiguity than that of low inclination, because contribution from asteroid belt is negligible and the source comets are visible(free from observational selection) through the whole course of orbital evolution.

Type
Part II - Comets and Meteor Streams
Information
International Astronomical Union Colloquium , Volume 74: Dynamical Trapping and Evolution in the Solar System , 1983 , pp. 97 - 104
Copyright
Copyright © Reidel 1983

References

Cowan, J.J. and A’Hearn, M.F. : 1979, The Moon and the Planets, 21, 155.Google Scholar
Everhart, E.: 1972, Astrophys. Letter, 10, 131.Google Scholar
Kresák, L.: 1980, The Moon and the Planets, 22, 83.Google Scholar
Levin, B.J. and Simonenko, A.N.: 1981, Icarus, 47, 487.CrossRefGoogle Scholar
Marsden, B.G., Sekanina, Z. and Yeomans, D.K.: 1973, Astron. J., 78., 211.Google Scholar
Marsden, B.G., Sekanina, Z. and Everhart, E.: 1978, Astron. J., 83, 64.Google Scholar
Marsden, B.G.: Catalogue of Cometary Orbits, 3rd Ed.(1979), Central Bureau of Astronomical Telegram, IAU.Google Scholar
Nakamura, T.: 1981, Icarus, 45, 529.Google Scholar
Öpik, E.J.: 1963, Advances Astron. Astrophys., 2, 219.CrossRefGoogle Scholar
Rahe, J.: Landoldt-Bornstein, New Series, Vol.2, Subvol.a, Methods, Contants, Solar System(Ed. by Schaifers, K. and Voight, H.H.), Chap.3, Springer-Verlag, Berlin(1981).Google Scholar
Rickman, H. and Froeschle, C.: 1980, The Moon and the Planets, 22, 125.CrossRefGoogle Scholar
Weissman, P.R. : 1980, Astron. Astrophys., 85, 191.Google Scholar
Wetherill, G.W.: 1979, Icarus, 37, 96.Google Scholar
Whipple, F.L.: Comets, in Cosmic Dust(Ed. by McDonnell, J.A.M. , Chap.l, John Wiley & Sons, New York(1978).Google Scholar