Tidal evolution of the Uranian satellites. III - Evolution through the Miranda-Umbriel 3:1, Miranda-Ariel 5:3, and Ariel-Umbriel 2:1 mean-motion commensurabilities

Details Tidal evolution of the Uranian satellites. III - Evolution through the Miranda-Umbriel 3:1, Miranda-Ariel 5:3, and Ariel-Umbriel 2:1 mean-motion commensurabilities Tidal evolution of the Uranian satellites. III - Evolution through the Miranda-Umbriel 3:1, Miranda-Ariel 5:3, and Ariel-Umbriel 2:1 mean-motion commensurabilities

Jun 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990icar...85..394t&link_type=abstract

Icarus (ISSN 0019-1035), vol. 85, June 1990, p. 394-443.

Physics

34

Eccentric Orbits, Orbital Elements, Orbital Resonances (Celestial Mechanics), Planetary Evolution, Tides, Uranus Satellites, Melting Points, Planetary Geology, Satellite Surfaces, Voyager 2 Spacecraft, Uranus, Satellites, Tides, Evolution, Miranda, Umbriel, Ariel, Motion, Orbital Elements, Orbits, Celestial Mechanics, Chaos, Tidal Effects, Eccentricity, Inclination, Resonance, Parameters, Dynamics, Models, Diagrams, Perturbations, Calculations, Friction

Scientific paper

Numerical experiments have been conducted which indicate that the orbital eccentricity of Miranda may have reached a value sufficiently large to have affected its thermal evolution. There is a large chaotic zone associated with the Miranda-Ariel 5:3 mean-motion commensurability, even in the planar approximation; the orbital eccentricities of both satellites may vary chaotically for a considerable period. Since the anomalously high orbital inclination of Miranda is a consequence of passage through the 3:1 commensurability with Umbriel, the requirement that the satellites encountered this resonance places a lower limit on the Uranian specific dissipation function of 39,000.

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