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• W2033136430 abstract "The distribution of hot spots on Io's surface and Io's figure constrain models of Io's interior. Voyager observations indicate that most hot spots and volcanic plumes are close to the equator. Recently, however, it has been proposed that a large low-albedo feature in the south polar region may be the source of 40% of the surface heat flow. We calculate spatial distributions of the dissipation rate, surface heat flow, and the figures of three- and four-layer, Maxwell rheology models of Io by using the correspondence principle. The models are required to satisfy the observed surface heat flow constraint and are consistent with the composition of a dehydrated C2-chondrite. They consist of an inviscid FeFeS core and viscoelastic silicate mantle and lithosphere layers. A comparison of the calculated equilibrium figure with the observed figure of Io supports the chosen core radius of 980 km. In addition, the four-layer model has a partially molten asthenosphere a few tens of kilometers thick. The preferred three-layer model has a mantle shear modulus of 1010 Pa and a viscosity of 2 × 1016 Pa s consistent with rock properties. The tidal dissipation rate for this model is largest along the polar axis. Integration of the dissipation rate over radius gives a surface heat flow with maxima at the poles and minima near the sub-Jovian and anti-Jovian points. In contrast, the dissipation rate in a molten or partially molten incompressible asthenosphere has maxima near the equator and is close to zero at the poles. The asthenosphere dissipation rate is mainly a function of asthenosphere viscosity and thickness; the thinner the asthenosphere the smaller is the required viscosity. A 50-km-thick asthenosphere requires a viscosity of about 108 Pa s. A strong south polar hot spot, if it can be confirmed by infrared observation, favors dissipation in the mantle but does not exclude dissipation in a partially molten asthenosphere. Equatorial hot spots and the concentration of Prometheus-type plumes near the equator favor asthenosphere heating but do not rule out deep mantle dissipation. Both asthenosphere and deep mantle heating may contribute to Io's surface heat flow. The properties of magma transport through the lithosphere and the planform of mantle convection might exert a control on the surface expression of heating at greater depth." @default.
• W2033136430 created "2016-06-24" @default.
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• W2033136430 date "1988-08-01" @default.
• W2033136430 modified "2023-09-23" @default.
• W2033136430 title "Tidal dissipation, surface heat flow, and figure of viscoelastic models of Io" @default.
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• W2033136430 doi "https://doi.org/10.1016/0019-1035(88)90001-2" @default.
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