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| Dynamical instabilities and the formation of extrasolar planetary systems |
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| Author(s): Rasio FA, Ford EB |
| Source: SCIENCE Volume: 274 Issue: 5289 Pages: 954-956 Published: NOV 8 1996 |
| Times Cited: 223 References: 18 |
| Abstract: The existence of a dominant massive planet, Jupiter, in our solar system, although perhaps essential for long-term dynamical stability and the development of life, may not be typical of planetary systems that form around other stars. In a system containing two Jupiter-like planets, the possibility exists that a dynamical instability will develop. Computer simulations suggest that in many cases this instability leads to the ejection of one planet while the other is left in a smaller, eccentric orbit. In extreme cases, the eccentric orbit has a small enough periastron distance that it may circularize at an orbital period as short as a few days through tidal dissipation. This may explain the recently detected Jupiter-mass planets in very tight circular orbits and wider eccentric orb its around nearby stars. |
| Document Type: Article |
| Language: English |
| Reprint Address: Rasio, FA (reprint author), MIT, DEPT PHYS, CAMBRIDGE, MA 02139 USA |
| Publisher: AMER ASSOC ADVANCEMENT SCIENCE, 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 |
| Subject Category: Multidisciplinary Sciences |
| IDS Number: VR792 |
| ISSN: 0036-8075 |
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| | | | | | | | | Record from Web of Science® | | | | | | | | | |