Viscoelastic relaxation of the lithosphere beneath the Martian polar caps: Implications for the polar caps formation history and planetary thermal evolution

Mars harbors two geologically young (<100 Ma) and large (~1000 km across) polar ice caps, which represent the only million-year-old surface features that induce measurable surface deformations. In the absence of in situ heat flow measurements, analyses of these deformations is one of the few methods that give access to the present-day planetary thermal state. The latter is indicative of the concentration of radiogenic elements in the interior, which is an important metric to determine the planets bulk composition, structure, and geologic evolution (Plesa et al., 2022). In previous work, we have imaged the deformed basements beneath the two polar caps and have determined the present-day thermal state of Mars (Broquet et al., 2020; 2021). The results of these studies are currently widely used as firm constraints on Martian thermal evolution models (e.g., Plesa et al., 2022). However, these models struggle to explain both the thick lithospheres inferred at the poles and the planets young volcanism and ongoing plume activity (e.g., Broquet Andrews-Hanna, 2023). Importantly, Broquet et al. have assumed the polar deformations to be at equilibrium, which is only valid if the time elapsed since the polar caps formation is greater than the time required for viscous adjustments. This assumption is central to these models and depends upon the poorly known age of the polar caps and the internal viscosity structure of Mars. In this work, we couple a novel viscoelastic modelling approach of the polar deformations to thermal evolution models that account for InSight seismic measurements and observational constraints on recent volcanic activity. Our preliminary investigations reveal that viscosity structures, outlined in the thermal models presented in Plesa et al. (2022), lead to polar deformations reaching equilibrium in a few Myr and up to hundreds of Myr. These findings demonstrate that viscoelastic relaxation can surpass the polar caps ages, emphasizing the necessity for a comprehensive exploration of polar viscoelastic relaxation. This approach will yield critical insights into the internal viscosity structure of Mars together with the polar caps' age and formation history, ultimately leading to a better understanding of the planets geologic and climatic evolution. Broquet A., et al., (2021). The composition of the south polar cap of Mars derived from orbital data. JGR:Planets 126, e2020JE006730. 10.1029/2020JE006730. Broquet A. et al., (2020). Flexure of the lithosphere beneath the north polar cap of Mars: Implications for ice composition and heat flow. GRL 47, e2019GL086746. 10.1029/2019GL086746. Broquet A., Andrews-Hanna J. C., (2023). Geophysical evidence for an active mantle plume underneath Elysium Planitia on Mars. Nat. Astro. 7, 160169. 10.1038/s41550-022-01836-3. Plesa A.-C., et al., (2022). Interior Dynamics and Thermal Evolution of Mars a Geodynamic Perspective. Adv. Geophys. 63, 179230. 10.1016/bs.agph.2022.07.005.