Origin and evolution of the Uranian and Neptunian satellites: Some dynamical considerations

Details Origin and evolution of the Uranian and Neptunian satellites: Some dynamical considerations Origin and evolution of the Uranian and Neptunian satellites: Some dynamical considerations

Oct 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984nascp2330..377d&link_type=abstract

In JPL Uranus and Neptune p 377-404 (SEE N85-11927 02-91)

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2

Evolution (Development), Natural Satellites, Neptune (Planet), Orbits, Uranus (Planet), Ariel, Celestial Mechanics, Miranda, Orbital Resonances (Celestial Mechanics), Planetary Rings, Roche Limit, Tides

Scientific paper

The satellite system of Neptune is so irregular that some formation mechanism or subsequent dynamical evolution that sets it apart from the other, more regular, satellite systems is obviously indicated. McKinnon has argued that satellite capture is the most likely possibility and has shown that tidal circularization of Triton's presumably highly eccentric initial orbit probably resulted in melting of the satellite's interior. The satellite system of Uranus, although somewhat bland, also has a number of special features that indicate an interesting dynamical history. These include the anomalously high orbital inclination of Miranda and the probable coexistence of small satellites and narrow rings inside the planet's Roche limit. The author discusses the possibility that orbital evolution due to tidal dissipation is involved in both of these phenomena. Other topics discussed are: the origin of rings; the formation of coorbital satellites; the lack of stable orbit-orbit resonances in the Uranian satellite system; and chaos, tidal heating and the shapes of Miranda and Ariel.

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