Dynamical instabilities and the formation of extrasolar planetary systems

Details Dynamical instabilities and the formation of extrasolar planetary systems Dynamical instabilities and the formation of extrasolar planetary systems

Nov 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996sci...274..954r&link_type=abstract

Science, vol. 274, p. 954-956

Other

320

Aerospace Sciences, Computerized Simulation, Planetary Systems, Planets, Solar System, Gravitation, Orbits, Stability, Units Of Measurement

Scientific paper

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 periastrom 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 orbits around nearby stars.

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