Melting of Io by Tidal Dissipation

  title={Melting of Io by Tidal Dissipation},
  author={Stanton J. Peale and Patrick M. Cassen and R. T. Reynolds},
  pages={892 - 894}
The dissipation of tidal energy in Jupiter's satellite Io is likely to have melted a major fraction of the mass. Consequences of a largely molten interior may be evident in pictures of Io's surface returned by Voyager I. 
Planetary science: Tidal flows in satellite oceans
Sub-surface oceans probably exist on several large satellites of Jupiter and Saturn. An analysis of Europa's tides suggests that some of the Rossby waves are resonantly enhanced by the obliquity,
The role of SO2 in volcanism on Io
Io and Earth are the only planetary bodies known to be volcanically active; the energetics of the eruptive plumes on Io have important structural implications and are closely linked with the presence
How tidal heating in Io drives the galilean orbital resonance locks
Tidal heating in Io is the most likely energy source of its volcanic activity. Tidal dissipation in Io and Jupiter also controls the resonance configuration among the three inner satellites. The
Volcanoes on Io
The tidal forcing phenomenon used to predict the existence of volcanic activity on Io, is treated from a very simple point of view which nevertheless reproduces to a sufficient accuracy the final
Ice-volcanism due to tidal stress on Europa
Tectonism would be driven by tidal heat on Europa, and there may be ice-volcano on the surface of active Europa. We assume that ice-volcano would spurt out due to tidal stress, and calculate the
Tidal dissipation at arbitrary eccentricity and obliquity
The stability of an SO2 atmosphere on Io
Measurements of Io's volcanism and the plasma torus suggest that SO2 is a major constituent of its atmosphere.
Structural and Thermal Icy Satellite Models: Preliminary Results
The satellites of the outer solar system appear to be composed principally of water ice and silicates, with the presence of ammonia and methane hydrates (Lewis 1971). Although these bodies are small
Is there liquid water on Europa
It is possible that tidal dissipation in an ice crust on Europa preserved a liquid water layer beneath it, provided that the three-body orbital resonance for Io, Europa, and Ganymede is ancient. The


Satellites of the Outer Planets: Thermal Models
The present-day steady-state thermal structure of a representative satellite, J IV (Callisto), is shown to be characterized by the presence of a thin icy crust over a deep liquid mantle, with a dense core of hydrous silicates and iron oxides.
Q in the solar system
Steady and transient thermal convection in a fluid layer with uniform volumetric energy sources
Measurements of the overall heat flux in steady convection have been made in a horizontal layer of dilute aqueous electrolyte. The layer is bounded below by a rigid zero-heat-flux surface and above
Io: An Intense Brightening Near 5 Micrometers
Spectrophotometric observations of the jovian satellite Io on 20 and 21 February 1978 (Universal Time) found that the 5-micrometer albedo of Io is near unity under ordinary conditions, so the observed transient phenomenon must have been the result of an emission mechanism.
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