Physics
Scientific paper
Apr 1978
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978m%26p....18..203n&link_type=abstract
Moon and the Planets, vol. 18, Apr. 1978, p. 203-216.
Physics
3
Gravitational Effects, Natural Satellites, Satellite Rotation, Secular Variations, Solar System, Tides, Angular Velocity, Energy Dissipation, Light Curve, Planetary Evolution, Planetary Orbits, Solar Orbits
Scientific paper
The tidal evolution of a planet-satellite system with zero eccentricity can be separated into two phases: phase 1 - from formation of the system to the time when the satellite begins to corotate, and phase 2 - after onset of corotation. Darwin's (1908) graphical method is applied to phase 1 for planet-satellite systems of the solar system. On the assumption that the spin angular velocity of the planet does not change from satellite corotation to the present, calculations are performed for the satellite's corotation distance and the time interval necessary to reach such a distance as a function of the satellite's Q. By setting this time interval to less than one billion years, an upper limit to a satellite's Q is obtained which determines whether or not it is corotating. A total of 21 satellites appear to corotate. Qualitative information on the future evolution of the corotating satellites is also obtained.
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