Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996dps....28.2132s&link_type=abstract
American Astronomical Society, DPS meeting #28, #21.32; Bulletin of the American Astronomical Society, Vol. 28, p.1140
Astronomy and Astrophysics
Astronomy
Scientific paper
The H2O band at around 1.6 mu m, whose shape is temperature dependent, shows promise as a tool for mapping the surface temperatures of the Galilean satellites with near-infrared spectrometers. The bands in this region becomes narrower and more pronounced at lower temperatures. Changes in the band are noticable between about 70 to 230 K. Kieffer and Smythe (Icarus, 1974) suggested using this feature to map the temperatures of the Galilean satellites. The temperature/band depth relationship was refined by Lebofsky. The NIMS experiment has sufficiently high spatial resolution at this wavelength to map the apparent surface temperatures in some detail. A simple ratio of the 1.6 and 2 mu m bands produces a map which appears to correlate well with expected temperatures - the poles are cold and bright areas are colder than dark areas. The area near Osiris appears colder than surrounding areas, including areas at earlier local hour angles. While the technique is promising, a detailed photometric correction needs to be applied before accurate temperatures can be derived, since the depth of bands and apparent width of absorption bands is also highly dependent on particle size and surface compaction.
Arakelian T.
Galileo NIMS Team
Smythe William
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