Io - Observational constraints on internal energy and thermophysics of the surface

Details Io - Observational constraints on internal energy and thermophysics of the surface Io - Observational constraints on internal energy and thermophysics of the surface

Nov 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980icar...44..226m&link_type=abstract

(IAU, American Astronautical Society, COSPAR, University of Hawaii, and NASA, Colloquium on the Satellites of Jupiter, 5th, Kail

Astronomy and Astrophysics

Astronomy

48

Infrared Astronomy, Internal Energy, Io, Satellite Surfaces, Thermal Emission, Thermophysical Properties, Brightness Temperature, Heat Transfer, Hot Surfaces, Infrared Spectra, Radiant Flux Density, Surface Properties

Scientific paper

Infrared observations of the Io eclipse of April 12, 1980, in five broad bands from 3 to 30 microns define the thermal emission spectrum both during and after eclipse. A substantial fraction of the emitted radiation during eclipse arises from hot spots; the equivalent global average heat flow is 1.5 + or - 0.3 W/sq m, corresponding to an internal source of (6 + or - 1) x 10 to the 13th W. The hot spot spectra can be matched by components with color temperatures of 200-600 K covering 1-2% of the surface. Comparison with observations over the past eight years suggests that, while the flux at the hottest temperatures may be highly variable, there is no evidence for major changes in the total heat flow, which is emitted primarily in the spectral region 10-20 microns. The heating curves of the surface were observed at 10 and 20 microns; when corrected for the hot spot contribution they indicate a typical global thermal inertia for Io of 0.0002 + or - 0.0001 cal/sq cm sec1/2 K, similar to that of the other Galilean satellites.

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