Mathematics – Logic
Scientific paper
Sep 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.5203k&link_type=abstract
American Astronomical Society, DPS meeting #38, #52.03; Bulletin of the American Astronomical Society, Vol. 38, p.579
Mathematics
Logic
1
Scientific paper
During the T13 Titan flyby on 2006 April 30, the Cassini RADAR obtained a synthetic aperture (SAR) image from 62 to 170 W longitude at 10 S latitude, crossing almost the entire 3600 km width of the IR-bright region Xanadu. The region is revealed to be remarkably rugged and different from the remainder of Titan seen so far. Earlier radiometric observations showed Xanadu to have low emissivity and very low polarization, suggesting a rough surface with low dielectric constant and significant volume scattering (Janssen et al., this conference). The T13 SAR data are consistent with these results, showing a radar-bright surface with backscatter almost independent of incidence. Morphologically, Xanadu is populated with ubiquitous, closely spaced hills 5 km across, which locally form chains and appear to be dissected by numerous channels and low areas filled by radar-dark sediments. Radarclinometry indicates typical hills are at least 500 m high, but the results are asymmetric, strongly suggesting that the foreshortened bright slopes are unresolved. If so, the hills are 1000 m high with 30 degree slopes. In either case Xanadu contrasts strongly with the rest of Titan, where topographic features are rare and mostly <300; m high. Information about relief over distances >20; km is limited, but Stiles et al. (this conference) offer evidence that Xanadu as a whole is quite flat. Comparison with VIMS data (Soderblom et al., this conference) suggests the surface is extensively coated with bright tholin deposits, with some variation in water ice content correlated with features in the SAR. We therefore hypothesize that Xanadu was formed by an initial period of compressive tectonism and cryovolcanism that triggered the erosion that sculpted the rugged surface, but that current erosion rates are very low, allowing a thicker coating of IR- and radar-bright material to accumulate than elsewhere on Titan.
Cassini RADAR Team
Janssen Michael A.
Kirk Randolph L.
Lopes Ricardo
Lorenz Ralph D.
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