Io's surface and environs - A magmatic-volatile model

Details Io's surface and environs - A magmatic-volatile model Io's surface and environs - A magmatic-volatile model

Oct 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979georl...6..799h&link_type=abstract

Geophysical Research Letters, vol. 6, Oct. 1979, p. 799-802. NASA-supported research.

Astronomy and Astrophysics

Astronomy

12

Io, Magma, Planetary Composition, Planetary Surfaces, Volatility, Absorption Spectra, Astronomical Models, Infrared Astronomy, Sulfur Compounds, Volcanoes, Io, Satellites, Surface, Models, Magmas, Volatiles, Physical Properties, Crust, Sulfur, Dissociation, Ice, Convection, Toruses, Absorption Spectra, Protons, Silica, Composition, Observations, Volcanic Features, Outgassing, Thermal Gradients, Sulfur Dioxide, Hydrogen Sulfide, Oxygen, Partial Pressure, Jupiter

Scientific paper

A model is proposed to account for the observed properties of Io. The crust is probably siliceous, but the outermost visible surface is composed primarily of several allotropes of elemental sulfur, plus frosts of SO2, H2S, and S2O. The 4-micron feature in Io's IR reflectance is identified as the (nu 1 + nu 3) band of SO2 frost. A possible source of the S is dissociation of iron sulfide brought up from the core by mantle convection. The SO2 is produced in the volcanoes, and the H2S by interaction of magnetospheric protons with the surface S. Delayed luminescence from S2O could cause the posteclipse brightening. The orbital torus is sustained by evaporation from molten ejecta from the volcanoes. Several additional diagnostic absorption bands and two additional minor torus species are predicted by this model.

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