Integrating THEMIS Imagery, MOC High-Resolution Images, and TES-Derived Thermal Inertia Data to Evaluate the Dust Thickness, Distribution, and Origin in the Tharsis Region and Arabia Terra, Mars

Details Integrating THEMIS Imagery, MOC High-Resolution Images, and TES-Derived Thermal Inertia Data to Evaluate the Dust Thickness, Distribution, and Origin in the Tharsis Region and Arabia Terra, Mars Integrating THEMIS Imagery, MOC High-Resolution Images, and TES-Derived Thermal Inertia Data to Evaluate the Dust Thickness, Distribution, and Origin in the Tharsis Region and Arabia Terra, Mars

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufm.p72a0489f&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #P72A-0489

Mathematics

Logic

5415 Erosion And Weathering, 5465 Rings And Dust, 5470 Surface Materials And Properties

Scientific paper

The Tharsis region and Arabia Terra, Mars are characterized as having a low albedo (0.26 to 0.35), low thermal inertia (26 to 148 J/m2Ks1/2), and low rock abundance. These regions are interpreted to be covered in a blanket of unconsolidated dust with an average particle size less than about 40 microns. Areas of low thermal inertia and high albedo are inferred to be regions of active dust accumulation and low wind velocities implying that the dust thickness is increasing. An understanding of the dust quantity on these surfaces and recent changes in dust thickness is critical to identify the erosional and depositional history of this deposit and to understand how recent geologic processes have affected the transport of fine-particulate material. The thickness of the dust deposits in the Tharsis region is currently estimated to be between 10 cm and several meters, with a reduction of thickness away from the center. Arabia Terra has a similar dust deposit and initial investigation suggests that the thickness of dust in this region is also variable. This study uses Mars Global Surveyor Thermal Emission Spectrometer (TES) thermal inertia information, Mars Orbiter Camera (MOC) high-angle images, and Mars Odyssey Thermal Emission Imaging System (THEMIS) infrared and visible data to quantitatively evaluate the distribution of dust and the variation in thickness of this deposit in Tharsis Montes and Arabia Terra, Mars. Thermal inertia will be used to calculate a minimum thickness of dust required to produce the thermal signature observed. MOC images will be analyzed via depth to diameter ratios of area craters and visual characteristics to assess the variation in dust mantling. These thermal and visual characteristics will be utilized to assess the behavior of this surface cover, verify if this deposit possesses similar characteristics in both regions, and determine if these deposits have fluctuated in recent history.

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