Copernicus Crater is a large, prominent lunar impact crater located on the Moon's near side. It is named after the Polish astronomer Nicolaus Copernicus, who developed the heliocentric model of the solar system in the 16th century. Copernicus Crater has a diameter of approximately 93 kilometers (58 miles) and is estimated to be about 800 million years old.
The geology of Copernicus Crater is characterized by its central peak, which rises to a height of about 1.2 kilometers (0.75 miles) above the crater floor. The peak is made up of uplifted rocks that were originally located deep beneath the surface of the Moon. These rocks were uplifted by the impact that formed the crater and are believed to be part of the Moon's ancient highlands crust.
The crater floor is covered by a dark, flat plain known as a mare. This mare material is relatively young, geologically speaking, and has a radiometric age of around 1.1 billion years. The mare material is composed of basaltic lava flows that flooded the crater after the impact. These lava flows originated from volcanic eruptions in the nearby Imbrium Basin.
The walls of Copernicus Crater are steep and rugged, with terraces and landslides visible in many places. The rocks here are believed to be part of the Moon's ancient highlands crust, similar to the rocks in the central peak. The walls of the crater have been eroded by various geological processes over time, including landslides, impact gardening, and erosion by micrometeoroids.
Copernicus Crater is one of the most studied craters on the Moon, and has been the focus of numerous scientific investigations over the years. It is a popular target for telescopic observation and has been imaged by numerous lunar orbiters and landers, including the Lunar Reconnaissance Orbiter (LRO) and the Apollo missions. Its geology provides important insights into the history and composition of the Moon, and has helped scientists better understand the processes that shaped our nearest celestial neighbor.
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