Physics – Geophysics
Scientific paper
May 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987icar...70..334g&link_type=abstract
Icarus (ISSN 0019-1035), vol. 70, May 1987, p. 334-347.
Physics
Geophysics
31
Galilean Satellites, Orbital Mechanics, Planetary Evolution, Resonance, Eccentric Orbits, Laplace Equation, Libration, Tides, Jupiter, Satellites, Evolution, Resonance, Celestial Mechanics, Motion, Tidal Effects, Eccentricity, Ganymede, Io, Heating, Europa, Stability, Diagrams, Calculations, Hypotheses, Geophysics, Surface, Sulfur
Scientific paper
The Laplace resonance among the inner three Galilean satellites (mean motions n1-3n2+2n3 = 0) has stable configurations in "deep resonance", i.e., where mean motions taken by pairs are in ratios very close to 2:1. The present satellite configuration, with the resonance variable φ ≡ λ1-3λ2+2λ3 stable at 180°, is unstable near this exact commensurability. But there is a continuous path of stable conditions branching from φ = 180° to higher and lower values of φ and toward very deep resonance, according to a theory extended to third order in orbital eccentricity. This path provides a track for tidal evolution of the system. Thus, scenarios involving evolution (probably episodic) from deep resonance are viable, and eliminate the requirement by the alternative equilibrium hypothesis for rapid tidal dissipation in Jupiter.
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