Remote Sensing Investigations of Lunar Surface Evolution
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2024
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The lunar regolith, a poorly sorted layer of impact-generated debris that coats the entirety of the lunar surface, underlies the boots of astronauts, composes a large portion of the lunar sample suite, and is the primary material scientists can study remotely. Therefore, understanding the nature and evolution of regolith is essential to planning future missions. This dissertation explores differences in rock and regolith evolution on diverse surfaces across the Moon using multispectral remote sensing data and impact craters. In Chapter 2, I demonstrate that the volcanic maria, which were once thought to be homogeneous, are diverse and were likely formed by a spectrum of emplacement conditions. Thus, the regolith on these diverse surfaces evolves variably depending on the properties of the parent rock. In Chapter 3, I show that the highlands, which cover most of the lunar surface, are blanketed by a thick regolith that is highly variable. The estimate of a 10-15 meter thick regolith at the Apollo landing sites has typically been taken to be representative of most of the highlands. However, my analysis of rocky craters reveals that 95% of the highlands are covered by regolith thicker than 50 meters. Finally, in Chapter 4, I show that highlands topography influences regolith maturity. Relatively immature regolith is more likely to occur atop high-standing topography, while mature regolith is more common on low-lying terrain. This is a key finding that is relevant to the upcoming Artemis missions, which will explore high topography at the lunar South Pole. My findings enable us to predict that Artemis astronauts will encounter regolith that is immature and possibly abnormally thin due to the catastrophic loss of material from topographic highs.
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Planetology, Impact Craters, Lunar Highlands, Lunar Volcanism, Moon, Planetary Science, Regolith
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136 pages
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