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- Title
REINTERPRETING THERMAL INERTIA FOR MAPPING MARTIAN GEOLOGY.
- Authors
Koeppel, Ari; Edwards, C. S.; Carrillo, G.; Annex, A.; Lewis, K.
- Abstract
Model-derived thermal inertias (TIs) have frequently been used to help distinguish geologic units in mapping efforts of the surface of Mars. Generally, higher TI values are associated with compacted surfaces and bedrock, while lower values are associated with poorly consolidated sediments and other friable deposits [1]. Our efforts to map layered sedimentary deposits within equatorial craters on Mars have revealed an inconsistent correlation between TI and geologic unit type [2]. Over areas where surface landform morphologies and VNIR spectra remain relatively constant, modeled TI sometimes varies dramatically. One possible explanation for the patterns in TI is that thin dust coatings have a strong influence on surface temperatures, and that dust accumulation is limited in very friable units and regions of high wind velocities by aeolian erosion [3]. If this is the case, it will force us to reassess how we use TI maps in geologic mapping. We tested the localized dust cover hypothesis by taking a statistical approach to uncovering nuanced relationships between mineral signals, crater densities, wind patterns and TI. We found that surface TI is frequently reduced on heavily cratered terrains and leeward slopes compared to crater-free surfaces containing erosional landforms (e.g. yardangs) and windward slopes. As a result, we suggest that geologic mapping efforts on Mars must consider local erosional patterns and abrasion susceptibility when using thermal inertia as a tool for differentiating geologic units.
- Subjects
MARTIAN geology; GEOLOGICAL mapping; GEOLOGICAL maps; MARTIAN craters; LUNAR craters; IMPACT craters; WIND speed
- Publication
LPI Contribution, 2021, p1
- ISSN
0161-5297
- Publication type
Article