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| Layers of material are exposed in Galilei crater's wall, sloping downward to bottom left. Each successive layer provides a step back in time and hints at the process that formed the layers of Oceanus Procellarum basin. LROC Narrow Angle Camera (NAC) observation M160363453LE, LRO orbit 8767, May 18, 2011; incidence angle 53.64° with a resolution of 0.48 meters per pixel from 40.77 kilometers. View the full 500 meter-wide original LROC Featured Image HERE [NASA/GSFC/Arizona State University]. |
LROC News System
Impact craters are a great resource for planetary scientists. Craters can be counted and used to age date a surface, they can tell us about the strength of the surface they formed in, and they can tell us about the composition of a surface at depth. Because they also expose bedrock in their crater walls, they can expose exciting geologic features.
In today's Featured Image, long continuous shelves can be seen in the steep walls of Galilaei crater! How did they form?
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| Context image of today's Featured Image, located within the white box (at the end of the long arrow). Galilaei crater is located in Oceanus Procellarum north of Reiner Gamma. 32 meter per pix resolution LROC QuickMap view HERE [NASA/GSFC/Arizona State University]. |
When Galilaei crater formed, the impacting bolide punched through a thick mare basalt. The lines define layers that are consistent in thicknesses and blockiness over large distances. Geologists have studied thick basalt deposits in great detail on the Earth. In most cases the terrestrial examples were formed as many lava flows stacked up one above the other. The layers seen in today's Featured Image are about the same thickness as those found in flood basalts on the Earth and found elsewhere on the Moon. Taken together, these observations favor the lava flow interpretation. Future astronaut geologists will surely visit such layered deposits, and confirm if they really are individual flows or not.
How many layers do you see in the full NAC frame?
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