Internal structure of Planum Boreum, from Mars advanced radar for subsurface and ionospheric sounding data

Details Internal structure of Planum Boreum, from Mars advanced radar for subsurface and ionospheric sounding data Internal structure of Planum Boreum, from Mars advanced radar for subsurface and ionospheric sounding data

Sep 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010jgre..11509003s&link_type=abstract

Journal of Geophysical Research, Volume 115, Issue E9, CiteID E09003

Computer Science

Sound

3

Planetary Sciences: Solid Surface Planets: Physical Properties Of Materials, Planetary Sciences: Solid Surface Planets: Ices, Planetary Sciences: Solid Surface Planets: Remote Sensing, Planetary Sciences: Solar System Objects: Mars, Structural Geology: Regional Crustal Structure

Scientific paper

An investigation of the internal structure of the ice-rich Planum Boreum (PB) deposit at the north pole of Mars is presented, using 178 orbits of Mars advanced radar for subsurface and ionospheric sounding data. For each radargram, bright, laterally extensive surface and subsurface reflectors are identified and the time delay between them is converted to unit thicknesses, using a real dielectric constant of 3. Results include maps of unit thickness, for PB and its two constituent units, the stratigraphically older basal unit (BU) and the stratigraphically younger north polar layered deposits (NPLD). Maps of the individual units' surface elevation are also provided. Estimates of water ice volume in each unit are (1.3 ± 0.2) × 106 km3 in PB, (7.8 ± 1.2) × 105 km3 in the NPLD, and (4.5 ± 1.0) × 105 km3 in the BU. No lithospheric deflection is apparent under PB, in agreement with previous findings for only the Gemina Lingula lobe, which suggests that a thick elastic lithosphere has existed at the north pole of Mars since before the emplacement of the BU. The extent of BU material in the Olympia Planum lobe of PB is directly detected, providing a more accurate map of BU extent than previously available from imagery and topography. A problematic area for mapping the BU extent and thickness is in the distal portion of the 290°E-300°E region, where MARSIS data show no subsurface reflectors, even though the BU is inferred to be present from other lines of evidence.

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