Presentation Information

[O09-P11]Landforms created by impact with mud targets★Invited Papers

*Ayako I Suzuki1, Ichiro Kumagai2, Kei Kurita3 (1.Toyo University, 2.School of Science and Engineering, Meisei University, 3.Eearth-Life Science Institute, Science Tokyo)

Keywords:

Mars,Impact crater,Impact experiment

Many impact craters on Mars are known to possess ejecta deposits that differ in morphology from those observed around impact craters on the Moon and Mercury; these are referred to as fluidized ejecta craters. Observations such as the presence of thick continuous ejecta at distances away from the rim, the continuous ejecta to divert around pre-existing topographic highs, and the broader extent of the continuous ejecta compared with that on Mercury suggest that ejecta released by the impact became fluidized by some mechanism and was emplaced as a ground-hugging gravity flow (e.g., Carr et al., 1977). However, the factor responsible for this fluidization has not yet been identified. Clarifying the formation process of Martian fluidized ejecta craters is important not only for understanding impact physics but also for constraining the paleoclimate of Mars.
Low-velocity impact experiments under atmospheric conditions using free-fall projectiles have shown that landforms may or may not form depending on the depth of the mud target (Takada et al., 2002) and its viscosity (Suzuki et al., 2024). In this presentation, we focus on the coefficient of restitution of the substrate and the ejecta curtain angle, and demonstrate how differences in these parameters lead to variations in the resulting landforms.