SHARAD Investigation of the Interaction Between Volcanism and Deep Water Release in Elysium Planitia, Mars

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[5419] Planetary Sciences: Solid Surface Planets / Hydrology And Fluvial Processes, [5470] Planetary Sciences: Solid Surface Planets / Surface Materials And Properties, [5480] Planetary Sciences: Solid Surface Planets / Volcanism, [6225] Planetary Sciences: Solar System Objects / Mars

Scientific paper

Situated between the equator and 12°N and extending from 130° to 180°E, Elysium Planitia is considered to be the youngest volcanic plain on Mars. Recent crater counts on individual lava units argue for multiple phases of activity over the last 230 Myrs, with the most recent volcanic features dating to just ~2 Ma. The region also contains the youngest outflow channels on the planet. Multiple channel systems which are present across the region are interpreted to have been carved by the release of deep ground water (>1 km) from the broadly east-west trending Cerberus Fossae graben system. Elysium Planitia is therefore a region of high scientific interest, as it represents an ideal site to investigate the interaction of lava and water both below and on the surface of Mars. Extensive geologic mapping of Elysium Planitia has provided detailed information concerning the stratigraphy of the major volcanic units in addition to the classification of other landforms attributed to volcanic (e.g. small shields), fluvial (e.g. outflow channels) and aeolian (e.g. yardangs) activity. Orbital sounding radar provides a means to take this work to the next level through the mapping of buried surfaces associated with a contrast in dielectric permittivity and thus can be used to investigate the 3-D structure of the subsurface. Previous studies using the SHARAD radar sounder onboard the Mars Reconnaissance Orbiter have identified multiple subsurface reflectors below the plains of Elysium Planitia. We will present our investigation of SHARAD data covering the eastern portion of this region of Mars - an area that includes the upstream reaches of Marte Vallis and the eastern extent of Cerberus Fossae. Our subsurface mapping shows remarkable correlations with published geologic maps produced using visible orbital datasets. These similarities allow us to use SHARAD data to make estimates of the average permittivity values and imply density measurements of the volcanic units. We will present these estimates and compare them to values derived over other young volcanic regions on Mars. Sounding radar provides the only type of orbital instrument to derive bulk estimates of geochemical properties of martian volcanic materials. Additionally we have identified the original fluvial eroded bed of Marte Vallis, prior to burial by younger lava flows. Through the mapping of the associated fluvial features we are able to tie the origin of Marte Vallis to Cerberus Fossae and provide further support for the recent (Late Amazonian) deep subsurface release of water on the surface of Mars. Our work will provide valuable constraints on the influence of recent volcanism on martian subsurface reservoirs of water.

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