Near-infrared spectral mapping of Titan's mountains and channels

Details Near-infrared spectral mapping of Titan's mountains and channels Near-infrared spectral mapping of Titan's mountains and channels

Nov 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007jgre..11211006b&link_type=abstract

Journal of Geophysical Research, Volume 112, Issue E11, CiteID E11006

Physics

34

Planetary Sciences: Solid Surface Planets: Surface Materials And Properties, Planetary Sciences: Solid Surface Planets: Hydrology And Fluvial Processes, Planetary Sciences: Solid Surface Planets: Instruments And Techniques, Planetary Sciences: Solid Surface Planets: Composition (1060, 3672)

Scientific paper

We investigate the spectral reflectance properties of channels and mountain ranges on Titan using data from Cassini's Visual and Infrared Mapping Spectrometer (VIMS) obtained during the T9 encounter (26 December 2005). We identify the location of channels and mountains using synthetic aperture radar maps obtained from Cassini's RADAR instrument during the T13 (30 April 2006) flyby. Channels are evident even in VIMS imaging with spatial resolution coarser than the channel size. The channels share spectral characteristics with Titan's dark blue terrain (e.g., the Huygens landing site) that is consistent with an enhancement in water ice content relative to the rest of Titan. We use this fact to measure widths of ~1 km for the largest channels. Comparison of the data sets shows that in our study area within the equatorial bright spectral unit east of Xanadu, mountains are darker and bluer than surrounding smooth terrain. These results are consistent with the equatorial bright terrain possessing a veneer of material that is thinner in the regions where there are mountains and streambeds that have likely undergone more recent and extensive erosion. We suggest a model for the geographic relationship of the dark blue, dark brown, and equatorial bright spectral units based on our findings.

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