摘要
Explores the scenario that the large random velocity (approx 5 km/s) among the asteroids is the result of dynamical interaction between the original population of the parent asteroids in near-circular orbits with some large planetesimals (JZB) scattered from the accretion zone of Jupiter. The statistical property of such a gravitational scattering process is evaluated using a Monte Carlo method. It is found that a few tens of JZB with individual masses reaching 3 X 1027 g would be needed to provide the necessary orbital velocity dispersion. -Author
原文 | ???core.languages.en_GB??? |
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頁(從 - 到) | 44-51 |
頁數 | 8 |
期刊 | Gerlands Beitrage zur Geophysik |
卷 | 96 |
出版狀態 | 已出版 - 1987 |