44-8 Geomorphological and Petrogenetic Analysis of Surface Features on Mars Using Remote Sensing Techniques

Session: Advancing Mineral Science and Exploring Planetary Surfaces: In Honor of MSA Dana Medalist, Elizabeth B. Rampe, Part II

Presenting Author:

Emma Mroz

Authors:

Mroz, Emma Natalyia¹, Sanchez, Veronica²

(1) Department of Physics & Geosciences, Texas A&M University-Kingsville, Kingsville, TX, USA, (2) Department of Physics and Geosciences, Texas A&M University - Kingsville, Kingsville, Tx, USA,

Abstract:

Mars has a complex geological history, particularly in the regions of Nili Fossae, Valles Marineris, and Sinus Meridiani, that provides critical insights into the past. This study focuses on the creation of a geodatabase to analyze the geomorphology of various regions across the surface of Mars, alongside the spatial distribution of key minerals such as olivine, hematite, and pyroxene to infer petrogenesis. We constructed a geodatabase using MOLA DEMs, TES global mineral abundance maps, CTX mosaics, and spectral data from the Mars Global Surveyor. Using ArcGIS Pro and JMars, we mapped variations in high-resolution visible and near-infrared spectral imagery. Surface analyses included topographic profiling, mapping surface features, and surface modeling with slope, aspect, and flow direction. Preliminary results suggest outflows containing olivine compose the abundant mineralogy of Nili Fossae within the graben of a prominent fault zone. In the Sinus Meridiani region, a large deposit of hematite is present with an association of olivine, which signifies an evident relationship between the two minerals, such as alteration. Within Valles Marineris, we observe plagioclase and high-Ca pyroxene within the walls of the canyon, hematite is found west in Noctis Labyrinthus, and in the eastern part of the canyon both olivine and hematite are detected. In the surrounding Tharsis Montes, several volcanoes within the region do not have olivine, hematite, pyroxene, or plagioclase exposed due to the surface dust coverage. D-Infinity flow direction indicates an outpouring of volcanic material into the Valles Marineris region and Solis Planum from the bordering Tharsis Montes. When comparing crustal thickness maps and the flow direction of mineral occurrences for Valles Marineris, we suggest volcanic activity might have been deeply sourced, further connecting to the dichotomy of crustal thickness. Across the southern hemisphere of Mars, the abundance of high-Ca pyroxene and plagioclase is also correlated to crustal dichotomy to suggest a deeper source for such mineralogy. Using the geodatabase to assess the geomorphology with the distribution of mineralogy is expected to further support a correlation to the paragenesis of minerals on Mars.

Geological Society of America Abstracts with Program. Vol. 57, No. 6, 2025

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