page_title: Beethoven (crater)
hierarchical_section_title: Beethoven (crater)
caption_attribution_description: English: Oblique view of Beethoven crater on Mercury. Approximate color representation combining three images acquired by MESSENGER Wide Angle Camera (EW0257129582I, EW0257129586F, EW0257129602G) with I (996.2 nm), G (748.7 nm), and F (433.2 nm) filters. Combined in GIMP software as RGB (Red-Green-Blue). Approximate north is up. Statistics for I image: Emission Angle: 34.0 Incidence Angle: 75.5 Latitude: -21.7 Longitude: 235.1 Phase Angle: 41.5
context_page_description: Beethoven is a crater at latitude 20°S, longitude 124°W on Mercury. It is 630 km in diameter and was named after Ludwig van Beethoven. It is the eleventh largest named impact crater in the Solar System and the third largest on Mercury.
  Unlike many basins of similar size on the Moon, such as the Orientale Basin, Beethoven is not multi-ringed. Remnant ejecta blankets around parts of the Beethoven are subdued in appearance and their margins poorly defined in places. The crater wall of Beethoven is buried by its ejecta blanket and by plains materials and is barely visible. The floor of the basin is covered with intermediate smooth plains material, which has the same reflectance as the exterior intermediate terrain. However, there are no wrinkle ridges or graben inside the basin like those in Caloris.
  Spudis and Prosser have suggested that Beethoven may possibly be late c3 in age or as old as early c2, which means that it is older than the Caloris Basin. The depth of Beethoven is estimated to be 2.5 ± 0.7 km from the stereo derived digital elevation models based on Mariner 10 images of the planet.
context_section_description: Beethoven is a crater at latitude 20°S, longitude 124°W on Mercury. It is 630 km in diameter and was named after Ludwig van Beethoven. It is the eleventh largest named impact crater in the Solar System and the third largest on Mercury (after Caloris and Rembrandt).
  Unlike many basins of similar size on the Moon, such as the Orientale Basin, Beethoven is not multi-ringed. Remnant ejecta blankets around parts of the Beethoven are subdued in appearance and their margins poorly defined in places. The crater wall (rim) of Beethoven is buried by its ejecta blanket and by plains materials and is barely visible. The floor of the basin is covered with intermediate smooth plains material, which has the same reflectance as the exterior intermediate terrain. However, there are no wrinkle ridges or graben inside the basin like those in Caloris.
  Spudis and Prosser have suggested that Beethoven may possibly be late c3 in age or as old as early c2, which means that it is older than the Caloris Basin. The depth of Beethoven is estimated to be 2.5 ± 0.7 km from the stereo derived digital elevation models based on Mariner 10 images of the planet. This is significantly less than the depth of lunar basins of the similar size indicating that Beethoven probably has relaxed from its post impact shape. There is also a broad topographic rise in the north–west margin of Beethoven.
caption: MESSENGER image of Beethoven
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