The formation of Tharsis on Mars: What the line‐of‐sight gravity is telling us

Abstract

Line‐of‐sight (LOS) spacecraft acceleration profiles from the Radio Science Experiment and topography from the Mars Orbiter Laser Altimeter (MOLA) instrument of the Mars Global Surveyor (MGS) are analyzed to estimate the effective elastic thickness (Te) for various regions of Tharsis. We identify a buried basin flanking the Thaumasia Highlands at the southeastern margin of Tharsis. Assuming that this basin results from lithospheric flexure from surface loading by the Thaumasia Highlands, we fit LOS profiles across the feature with a thin‐shell, elastic flexure model and find the mountain belt to reflect a value of Te ∼ 20 km consistent with a Noachian formation age. We also determine admittances from LOS profiles for five regions across Tharsis and fit them with theoretical admittances calculated using the flexural model. Crater density, surface density, and predominant surface age are found to vary systematically across Tharsis while Te does not. The highest surface density and lowest Te values are obtained for the western portion of Tharsis where crater densities are lowest. Our results imply the majority of the topographic rise was emplaced within the Noachian irrespective of the surface ages. Topographic loading and resurfacing (i.e., volcanic activity) persisted into the Amazonian while becoming increasingly confined to the western margin where the youngest surface ages are found and the eruptive style transitioned from effusive volcanism to shield‐forming volcanism as Te increased.