Mathematics – Logic
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufm.p33e1798l&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #P33E-1798
Mathematics
Logic
[6281] Planetary Sciences: Solar System Objects / Titan
Scientific paper
Titan's Xanadu region is one of the most fascinating, continent-sized surface features, hosting many kinds of geologic features, such as craters, channels, candidate paleolakes, mountain chains, and potential cryovolcanic flows. However, the geologic development of this region is still controversially debated. This study aims to verify current concepts about the development of Xanadu, while the main focus will be to test the idea of the genesis of western Xanadu by an ancient impact, proposed by Brown et al. (2011). The outer boundary of the Xanadu Circular Feature (XCF) is obvious through a large circular marking, 1,800 km across, seen in VIMS-data (Brown et al. 2011). According to Brown et al. (2011), radar-SAR data confirm the presence of an inner and outer boundary of that presumptive impact crater through differences in radar brightness. Further arguments supporting an impact origin are (amongst others, from Brown et al. 2011) the low brightness temperature of the region at 2.2 cm wavelength and its low topographic level. This study aims to extend and verify these findings based on current Cassini VIMS-, RADAR-SAR, and SAR-Topo data covering the Xanadu-region. VIMS data obtained at different times and at different viewing and illumination conditions, e.g. Cassini Orbit 22 (March 18, 2006) and Orbit 97 (Dec. 21, 2008), confirm the relative permanence of the outer margins of the XCF. Some parts of its putative outer boundary are visible in Radar-SAR, which confirms a correlation between VIMS and RADAR, possibly due to the presence of an outer boundary of an impact structure. Further, SAR-Topo data partly reproduce the southern (outer) boundary of the XCF and thus its topographic depression. Other confirming structures are the possible remains of radial and concentric features near the outer boundary of the XCF, visible in radar. Potential impact-induced cryovolcanic features are located at southern Xanadu, namely Tui Regio and Hotei Regio (e.g. Soderblom et al 2009, Wall et al 2009). A possible argument against an impact origin of western Xanadu is the fact that only fragments of the presumptive inner and outer boundaries of the XCF are visible in radar-SAR. Instead, the surface shows rather lobate shaped sections or patches of a radar-dark tone enclosed by rugged terrain (see Radebaugh et al. 2011, their Fig. 3). Further, the presence and orientation of mountain chains in Titan's equatorial region can be explained by alternative processes, such as contractional tectonism (e.g. Mitri et al. 2010). Radial and circular tectonic structures are not significantly accumulated within the margins of the potential impact feature, weakening the idea of an ancient impact in that region. The geology of the western Xanadu region will be compared to giant impact craters on Callisto and Ganymede. In contrast to the Jovian satellites, Titan's active methane cycle has to be taken into account in that comparison, since Titan's geologic features are exposed to erosion and presumably more short-lived than features on most other Solar System bodies.
Langhans M. H.
Lunine Jonathan I.
Mitri Giuseppe
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