Computer Science – Sound
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufm.p23a1625h&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #P23A-1625
Computer Science
Sound
[5400] Planetary Sciences: Solid Surface Planets, [5422] Planetary Sciences: Solid Surface Planets / Ices, [5494] Planetary Sciences: Solid Surface Planets / Instruments And Techniques, [6225] Planetary Sciences: Solar System Objects / Mars
Scientific paper
Martian hydrogeologic surface chronology strongly depends on our understanding of the cratering process and our ability to perform surface crater count to assess rough formation ages. Of particular interest are Isidis and Amazonis Planitia as both basins are among the smoothest surface areas on Mars with very few observable large craters. Such surface conditions give a unique potential to the current sounding radars to overcome clutter arising from surface textural and topographic complexity to assess the dielectric properties of the shallow subsurface and also to attempt to explore potential buried large craters that could constrain the ambiguities on the chronology and type of sedimentation that filled these two basins. Isidis has been hypothesized to be filled by either sediments derived from drainage leading into those lower topographic zones or by an older paleo-ocean. It has been suggested that those large-scale sedimentary deposits may still be volatile-rich. The Gamma Ray Spectroscopy Observations onboard Mars Odyssey suggested a maximum inferred water abundance of 3wt% in the top few meters. For Amazonis Planitia, it has been hypothesized that Tharsis produced lava flows that formed a barrier across the plain, which in turn created a basin that collected lava flows and other sediments. It is assumed that this basin and the repeated flows of lava and sedimentary materials through it, causing the smoothness of the plain, especially in the southern part of the basin. In order to constrain the chronology, origin and type of each of these basin fills, we created three-dimensional regional-normalized attenuation maps of the surface and shallow subsurface using the signal-decay method to provide insights into the three-dimensional variations of dielectric properties within these terrains. MARSIS radar tomography on Isidis yielded a complex large-scale westward flow-like pattern and ponding that appears to be similar to many of earth dry lakes. The attenuation were correlated to the MOLA topography, with the lower parts in the south of the basin being more conductive than the surrounding high lands suggesting that the basin fill have a different bulk composition from its surrounding geological unit. On Amazonis, 22 MARSIS orbits acquired over more than a year on the area from 6 to 8.3 N and from 170 to 172 E show a well-distinguished circular attenuation pattern in the first 400 meters that cannot be correlated to any feature of the surface topography, neither to ionospheric anomalies suggesting its source to be from an attenuation of a bowl-shape structure that we hypothesis to be a buried crater or lava lake.
Arellano Ferro Armando
Boisson Joséphine
Clifford Stephen M.
Gim Yonggyu
Heggy Essam
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