The Concentric Maclaurin Spheroid method with tides and a rotational enhancement of Saturn's tidal response

Abstract

We extend to three dimensions the Concentric Maclaurin Spheroid method for obtaining the self-consistent shape and gravitational field of a rotating liquid planet, to include a tidal potential from a satellite. We exhibit, for the first time, the important effect of the planetary rotation rate on tidal response of gas giants. Simulations of planets with fast rotation rates like those of Jupiter and Saturn, exhibit significant changes in calculated tidal love numbers $k_{nm}$ when compared with non-rotating bodies. A test model of Saturn fitted to observed zonal gravitational multipole harmonics yields $k_2=0.413$, consistent with a recent observational determination from Cassini astrometry data (Lainey et al., 2016). The calculated love number is robust under reasonable assumptions of interior rotation rate, satellite parameters, and details of Saturn's interior structure. The method is benchmarked against several published test cases.

40 pages, 8 figures, 3 tables

References in corpus (4)

• New constraints on Saturn's interior from Cassini astrometric data
• Phase separation in hydrogen-helium mixtures at Mbar pressures
• On the equilibrium figure of close-in planets and satellites
• The flattenings of the layers of rotating planets and satellites deformed by a tidal potential

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