Depletion of the outer asteroid belt

Science

Volumn 275, Issue 5298, 1997, Pages 375-377

  Liou, Jer Chyi ^a   Malhotra, Renu ^b  

^a NASA JOHNSON SPACE CENTER   (United States)

^b LUNAR AND PLANETARY INSTITUTE   (United States)

Author keywords

[No Author keywords available]

Indexed keywords

ARTICLE; ASTRONOMY; EVOLUTION; GRAVITY; MOTION; PRIORITY JOURNAL; ROCK; SUN;

ASTEROID; SPATIAL DISTRIBUTION; TEMPORAL VARIATION;

EID: 0030905245     PISSN: 00368075     EISSN: None     Source Type: Journal    
DOI: 10.1126/science.275.5298.375     Document Type: Article

References (21)

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3. R. Greenberg and H. Scholl, in Asteroids, T. Gehrels, Ed. (Univ. of Arizona Press, Tucson, 1979), pp. 310-333; A. M. Nobili, in Asteroids II. R. P. Binzel, T. Gehrels, M. S. Matthews, Eds. (Univ. of Arizona Press, Tucson, 1989), pp. 862-879.
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17. H from a planet, the dominant perturber is the planet, not the sun. The Hill radii of Jupiter and Saturn are 0.36 and 0.44 AU, respectively.
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19. R. Malhotra, unpublished material.
20. Because of the geometric locations of the 4:7, 3:5, and 5:8 interior MMRs, Jupiter has to migrate inward, by about 0.2 AU, to remove asteroids in the 3.5-to 3.9-AU region, However, the migration time scale and the migration scheme (linear, exponential, or other) are less constrained on the basis of the population of asteroids in this region. The long-term dynamics of the asteroids at 2:3 and 1:2 interior MMRs after the planet migration ceased may provide more insight into these questions.
21. We thank H. Zook for enthusiastic discussions. This research was performed while J.-C.L. held a National Research Council-NASA Johnson Space Center Research Associateship and R.M. was a staff scientist at the Lunar and Planetary Institute (LPI), which is operated by the Universities Space Research Association under contract NASW-4574 with NASA. Support was also provided by NASA's Origins of Solar Systems Research Program under grant 4474. This paper is LPI contribution 905.