INTERIOR MORPHOLOGY OF LUNAR PITS
Overhangs: Our models extend 10 m under the east rim of the Mare Tranquillitatis pit (MTP), and 15 m under the southwest rim of the Mare Ingenii pit (MIP). In both cases, the floor slopes downward under the overhang, indicating that debris may not have fully filled in the original void space. The Marius Hills (MHP) and Lacus Mortis pits, by contrast, do not have significant overhangs on the modeled walls and have flat or upward-sloping floors, suggesting a more complete infilling. In the case of MHP, the rim shows no evidence of extensive mass wasting to produce that infill, suggesting that either the original void space was very small or that the as-yet-unimaged west wall should have a significant opening.
Layering: We have measured the 3D locations of apparent morphological layer boundaries within the walls of MIP and MTP. We found good correspondence between layers on east and west walls and found median layer thickness of ~3.7 m in both MTP and MIP [3]. Additionally, MTP has a >8 m deep recess on the west, north, and possibly east walls at 40 m depth, suggesting a strength discontinuity - possibly evidence of a buried pyroclastic or paleoregolith layer.
[1] Haruyama et al. (2009), Geophys. Res. Lett. 36, L21206. doi:10.1029/ 2009GL0406355.
[2] Wagner and Robinson (2014), Icarus, 237C, 52–60. doi:10.1016/j.icarus.2014.04.002.
[3] Wagner and Robinson (2019), 50th LPSC, #2138.