A disk of scattered icy objects and the origin of Jupiter-family comets

Science

Volumn 276, Issue 5319, 1997, Pages 1670-1672

  Duncan, Martin J ^a   Levison, Harold F ^b  

^a QUEEN S UNIVERSITY   (Canada)

^b SOUTHWEST RESEARCH INSTITUTE   (United States)

Author keywords

[No Author keywords available]

Indexed keywords

ARTICLE; ASTRONOMY; EVOLUTION; MATHEMATICAL MODEL; PRIORITY JOURNAL; SIMULATION;

EVOLUTION, PLANETARY; ICE; JUPITER; METEOROIDS; NEPTUNE; SOLAR SYSTEM;

COMET; OUTER SOLAR SYSTEM;

JUPITER; NEPTUNE;

EID: 0030618767     PISSN: 00368075     EISSN: None     Source Type: Journal    
DOI: 10.1126/science.276.5319.1670     Document Type: Article

References (32)

1. j is the mean orbital velocity of Jupiter around the sun. JFCs typically have semi-major axes < 7 AU and perihelion distances less than 3 AU. Their mean inclination is ∼10°.
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16. This behavior can also be seen in figure 5 of M. Holman and J. Wisdom, Astron. J. 105, 1987 (1993). This earlier work demonstrates that the basic processes of temporary capture into mean motion resonance are not dependent upon the details of how we integrated close encounters in our simulation.
17. To first order, the orbit of a particle has two precessions associated with it. The first is the precession of the location where the orbit crosses the plane of the solar system (known as node-crossing). The second is the precession of the longitude of perihelion. The Kozai resonance [Y. Kozai, Astron. J. 67, 591 (1962)] occurs when the rate of these two precessions are the same. When a particle is in the Kozai resonance, it generally will not cross the plane of the solar system when it is at perihelion. Thus, particles with perihelion distances near Neptune will be protected from encounters with Neptune by the Kozai resonance.
18. We define a "visible" JFC as one with a perihelion distance < 2.5 AU. See (6) above for more details.
19. The observed population of JFCs suffers from observational biases, particularly with regard to a comet's perihelion distance and absolute magnitude. To perform a comparison between the results of our simulations and observations, we must correct for observational selection effects. A complete analysis is beyond the scope of this paper and we adopt the results in (6).
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31. -12 Earth masses [P. R. Weissman, Geol. Soc. Am. Spec. Pap 247, 263 (1990)]. This value is uncertain, because the size distribution is poorly determined.
32. We are grateful to S. Tremaine, who motivated this line of inquiry. We also thank L. Dones, B. Marsden, A. Stern, B. Gladman, M. Holman, W. Merline, and P. Weissman for comments on this manuscript. H.F.L. acknowledges grants provided by the NASA Origins of Solar Systems and Planetary Geology and Geophysics Programs. M.J.D. is grateful for the continuing financial support of the Natural Science and Engineering Research Council of Canada and for financial support for work done in the U.S. from NASA Planetary Geology and Geophysics Programs. We also acknowledge funding for our computer equipment from the National Science Foundation and the Southwest Research Institute.