Physics
Scientific paper
Jun 1979
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979natur.279..767y&link_type=abstract
Nature, vol. 279, June 28, 1979, p. 767-770.
Physics
66
Galilean Satellites, Jupiter (Planet), Orbital Mechanics, Orbital Resonances (Celestial Mechanics), Tides, Dissipation, Gravitational Effects, Orbit Calculation, Orbital Elements, Io, Jupiter, Satellites, Orbits, Resonance, Models, Heating, Voyager 1, Volcanoes, Europa, Ganymede, Perturbations, Damping, Velocity, Eccentricity, Librations, Gravitational Fields, Saturn, Enceladus, Dione, Three Body Problem, Thermal History
Scientific paper
The mechanisms by which orbital resonance locks are maintained among Io, Europa and Ganymede are analyzed, and the effects of the dissipative tides in Jupiter and Io on their establishment and evolution are considered. According to the proposed model, initially all three satellites are in orbits far from the 2:1 commensurabilities or the three body lock. The tide raised on Io damps down the free eccentricity; only modest tidal heating occurs. Subsequently the dissipative tide raised on Jupiter by Io causes Io's orbit to spiral outwards; Io approaches the 2:1 commensurability with Europa. Io's forced eccentricity increases rapidly to a critical value, and thereafter the resonant interaction causes Europa's orbit to expand at half that of Io's orbit. A fluid core is probably formed as the result of tidal heating. Finally Europa approaches the 2:1 commensurability, angular momentum is transferred from Europa's orbit to Ganymede's, and a steady state is attained. On the basis of the observed three-body resonance amplitude (0.066 deg), it is concluded that three-body resonance may have formed less than 500 million years ago; a measurement of the rate of tidal heating in Io may determine the Q value of both Io and Jupiter. Upper and lower limits for the Jovian Q value of 2 million and 20,000 are suggested.
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