Tidal Dissipation and Stability of the Laplace Resonance in the Galilean Satellites

Details Tidal Dissipation and Stability of the Laplace Resonance in the Galilean Satellites Tidal Dissipation and Stability of the Laplace Resonance in the Galilean Satellites

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufm.p12b0496m&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #P12B-0496

Physics

5450 Orbital And Rotational Dynamics, 5770 Tidal Forces, 6218 Jovian Satellites

Scientific paper

We present revisions to previous calculations of tidal dissipation in the Galilean satellites. Numerical simulations show that the evolution of the orbital elements in the two-dimensional model is very different from the evolution obtained with a three-dimensional model that also includes the Sun and Saturn, in addition to Jupiter and the four satellites. A new expression for the tidal dissipation valid to second order in eccentricity and for arbitrary inclination is therefore derived. Numerical simulations with values of ν (ν =2n2-n_1= 2n3-n_2=-0.74o/ day), increasing from the current value to ν =0.5, are carried out in order to check the stability of the Laplace resonance. Since the preliminary results show instability of the resonance and chaotic evolution of the eccentricity and inclination for ν =0 and for values that are very near to the deep resonance condition (e.g., ν =0.001, ν =0.01) further integrations are required to investigate the behavior of the system in deeper resonance. >http://geodyn.ess.ucla.edu/~musotto/abstractagu.html

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