As NASA continues to make progress toward sending astronauts to the lunar South Pole region with its Artemis campaign, data from a NASA-funded study is helping scientists better understand this strategic part of the Moon. The study presents evidence that moonquakes and faults generated as the Moon’s interior gradually cools and shrinks are also found near and within some of the areas the agency identified as candidate landing regions for Artemis III, the first Artemis mission planned to have a crewed lunar landing.
The epicenter of one of the strongest moonquakes recorded by the Apollo Passive Seismic Experiment was located in the lunar south polar region. However, the exact location of the epicenter could not be accurately determined. A cloud of possible locations (magenta dots and light blue polygon) of the strong shallow moonquake using a relocation algorithm specifically adapted for very sparse seismic networks are distributed near the pole. Blue boxes show locations of proposed Artemis III landing regions. Lobate thrust fault scarps are shown by small red lines. The cloud of epicenter locations encompasses a number of lobate scarps and many of the Artemis III landing regions. Image credit: NASA/LROC/ASU/Smithsonian Institution
“Our modeling suggests that shallow moonquakes capable of producing strong ground shaking in the south polar region are possible from slip events on existing faults or the formation of new thrust faults,” said Tom Watters of the Smithsonian Institution, Washington, lead author of a paper on the research published in the Planetary Science Journal. “The global distribution of young thrust faults, their potential to be active, and the potential to form new thrust faults from ongoing global contraction should be considered when planning the location and stability of permanent outposts on the Moon.”
Lunar Reconnaissance Orbiter Camera (LROC), Narrow Angle Camera (NAC) mosaic of the Wiechert cluster of lobate scarps (left pointing arrows) near the lunar south pole. A thrust fault scarp cut across an approximately 1-kilometer (0.6-mile) diameter degraded crater (right pointing arrow). Image credit: NASA/LRO/LROC/ASU/Smithsonian Institution
The Lunar Reconnaissance Orbiter Camera onboard NASA’s Lunar Reconnaissance Orbiter (LRO) has detected thousands of relatively small, young thrust faults widely distributed in the lunar crust. The scarps are cliff-like landforms that resemble small stair-steps on the lunar surface. They form where contractional forces break the crust and push or thrust it on one side of the fault up and over the other side. The contraction is caused by cooling of the Moon’s still-hot interior and tidal forces exerted by Earth, resulting in global shrinking.
The lobate scarps are formed when the lunar crust is pushed together as the Moon contracts. This causes the near-surface materials to break forming a thrust fault. The thrust fault carries crustal materials up and sometimes over adjacent crustal materials. Slip events on existing faults or the formation of new thrust faults trigger shallow moonquakes that can cause strong seismic shaking tens of miles (many tens of kilometers) away from the scarp. Image credit: Arizona State University/Smithsonian
The formation of the faults is accompanied by seismic activity in the form of shallow-depth moonquakes. Such shallow moonquakes were recorded by the Apollo Passive Seismic Network, a series of seismometers deployed by the Apollo astronauts.
The strongest recorded shallow moonquake had an epicenter in the south-polar region. One young thrust-fault scarp, located within the de Gerlache Rim 2, an Artemis III candidate landing region, is modeled in the study and shows that the formation of this fault scarp could have been associated with a moonquake of the recorded magnitude.
The team also modeled the stability of surface slopes in the lunar south polar region and found that some areas are susceptible to regolith landslides from even light seismic shaking, including areas in some permanently shadowed regions. These areas are of interest due to the resources that might be found there, such as ice.
Image shows predicted areas of surface slope instability in the south polar region. Models are for a one-meter-thick (about 3.3-foot) regolith landslide. Blue dots are areas with the least unstable slopes, green dots are moderately unstable slopes, and red dots are most unstable slopes. Image centered on Shackleton crater and the lunar south pole. Locations of proposed Artemis III landing regions are shown by the blue boxes. The model predicts large portions of the interior walls of Shackleton crater are suspectable to landslides (inset) as well as portions of interior crater walls in the Nobile Rim 1 landing region. Image credit: NASA/LROC/ASU/Smithsonian Institution
