Large-scale topography of Io - Implications for internal structure and heat transfer

Details Large-scale topography of Io - Implications for internal structure and heat transfer Large-scale topography of Io - Implications for internal structure and heat transfer

Jun 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988georl..15..581g&link_type=abstract

Geophysical Research Letters (ISSN 0094-8276), vol. 15, June 1988, p. 581-584.

Physics

34

Heat Transfer, Io, Satellite Imagery, Stereophotography, Topography, Voyager 1 Spacecraft, Altimetry, Lithosphere, Tectonics, Jupiter, Satellites, Io, Topography, Interior, Structure, Heating, Spacecraft Observations, Voyager 1 Mission, Imagery, Image Processing, Techniques, Thermal Effects, Lithosphere, Asthenosphere, Heat Flow, Thickness, Elevation, Crust, Models, Danube Planum

Scientific paper

Recent stereographic methods have been applied to Voyager 1 images in order to determine the shape and large-scale topography of Io. The best triaxial figure of semiaxes of 1830.0, 1818.7, and 1815.3 kilometers is consistent with a differentiated satellite in hydrostatic equilibrium. It is suggested that many of the broad topographic swells and basins noted may be due to isostatic responses to thermal changes in the lithosphere-asthenosphere system. Results support the picture of increasing heat flow converting the basal lithosphere into a lower-density asthenosphere, resulting in isostatic uplift. It is shown that lithospheric thicknesses ranging from 5-100 km may results in elevation variations of up to 1 km.

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