Measuring Regolith Depth across the Lunar Surface

Mathematics – Logic

Scientific paper

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[5470] Planetary Sciences: Solid Surface Planets / Surface Materials And Properties, [6250] Planetary Sciences: Solar System Objects / Moon

Scientific paper

Using new images captured from the Lunar Reconnaissance Orbiter Camera (LROC), we studied the lunar regolith depth at various locations across the Moon. Previous studies of regolith depth only examined the equatorial nearside of the Moon. With the global coverage of the new LROC images, we obtained regolith depth measures across the entire lunar surface, including the farside of the Moon and high latitude regions. Oberbeck and Quaide (JGR 1968) calculated the regolith depth of nearside equatorial regions such as Hipparchus (16m), Ocean Procellarum (3.3m), and Mare Tranquillitatis (4.6m). We used Oberbeck and Quaide’s method (JGR 1968) to calculate each region’s regolith depth. We located small (50 m diameter), flat-bottomed craters within each region. Measuring both the diameter of the flat-bottom feature and the diameter of the crater, we were able to calculate the regolith depth at each location using an equation empirically derived by Oberbeck and Quaide (JGR 1968) in their original experiments. Our results confirm the original results of Oberbeck and Quaide where our data overlap. We expanded on their work by examining new regions, including more nearside areas as well as areas in the high latitudes and on the farside of the Moon. Highland regions generally have deeper regolith than mare regions. We also compared regolith depths on adjacent, distinct geologic units; however, within these small regions, we found no statistically significant variation in regolith depth. By comparing the regolith depth across the lunar globe at varying scales, we gain a more thorough understanding of the cratering process and the geological evolution of the lunar surface.

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