Investigating the Cause of Moving Albedo Boundaries in the Oxia Palus Region of Mars

Details Investigating the Cause of Moving Albedo Boundaries in the Oxia Palus Region of Mars Investigating the Cause of Moving Albedo Boundaries in the Oxia Palus Region of Mars

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufm.p51b1427m&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #P51B-1427

Physics

[5415] Planetary Sciences: Solid Surface Planets / Erosion And Weathering, [6225] Planetary Sciences: Solar System Objects / Mars

Scientific paper

Recent imagery from the MARCI camera on Mars Reconnaissance Orbiter (MRO) in addition to previous analyses of Mars Global Surveyor MOC data reveals a variety of large scale changes in the appearance of the Martian surface (Geissler and Mukherjee, this meeting). The MOC and MARCI data revealed a surprising range of behavior in various regions of Mars. Our area of focus is a region featuring such albedo changes in Oxia Palus in western Arabia Terra. The albedo boundary between dark and bright terrain at western Oxia Palus moved 26 km eastwards between a MOC mosaic from September 2005 and a MARCI mosaic from July 2009. The goal of this project is to understand what is causing this albedo boundary to move. A distinctive feature of the Oxia Palus albedo boundary is a narrow (~25 km wide) fringe of locally high albedo that shifts as the boundary advances from the dark region (Acidalia) towards the bright terrain (Oxia). High resolution images from MRO’s CTX and HiRISE cameras will be used to test the hypothesis that the high albedo fringe is a coating of bright dust that is stripped by the winds from the advancing dark terrain and deposited ahead of the moving boundary.

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