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The moment of inertia of a giant planet reveals important information about the planet’s internal density structure and this information is not identical to that contained in the gravitational moments. The forthcoming Juno mission to Jupiter might determine Jupiter’s normalized moment of inertia NMoI=C/MR 2 by measuring Jupiter’s pole precession and the Lense–Thirring acceleration of the spacecraft...
We present ‘empirical’ models (pressure vs. density) of Saturn's interior constrained by the gravitational coefficients J2, J4, and J6 for different assumed rotation rates of the planet. The empirical pressure–density profile is interpreted in terms of a hydrogen and helium physical equation of state to deduce the hydrogen to helium ratio in Saturn and to constrain the depth dependence of helium and...
Pre-Cassini images of Saturn's small icy moon Enceladus provided the first indication that this satellite has undergone extensive resurfacing and tectonism. Data returned by the Cassini spacecraft have proven Enceladus to be one of the most geologically dynamic bodies in the Solar System. Given that the diameter of Enceladus is only about 500 km, this is a surprising discovery and has made Enceladus...
Doppler data generated with the Cassini spacecraft's radio carrier waves at X- and Ka-bands can be used to determine the quadrupole moments of Rhea's gravitational field. The resulting tri-axial field should be consistent with the assumption that Rhea is in tidal and rotational equilibrium. If so, we can construct interior models that are consistent with Rhea's mean density of 1236kg/m 3 ,...
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