Lunar Orbiter 4 image
|Colongitude||12° at sunrise|
Eratosthenes is a relatively deep lunar impact crater that lies on the boundary between the Mare Imbrium and Sinus Aestuum mare regions. It forms the western terminus of the Montes Apenninus mountain range. The crater has a well-defined circular rim, terraced inner wall, central mountain peaks, an irregular floor, and an outer rampart of ejecta. It lacks a ray system of its own, but is overlain by rays from the prominent crater Copernicus to the south-west.
At low Sun-angles this crater is prominent due to the shadow cast by the rim. When the Sun is directly overhead, however, Eratosthenes visually blends into the surroundings, and it becomes more difficult for an observer to locate it. The rays from Copernicus lie across this area, and their higher albedo serves as a form of camouflage.
In 1851 Shropshire Astronomer Henry Blunt constructed a model of the moon's surface showing Eratosthenes. The model is based on observations made by Blunt with a reflecting telescope from his home in Shrewsbury and was displayed in the same year at the Great Exhibition, London.
In 1924, William H. Pickering noted dark patches in the crater that varied in a regular manner over each lunar day. He put forward the speculative idea that these patches appeared to migrate across the surface, suggestive of herds of small life forms. The idea received a degree of attention primarily due to Pickering's reputation.
By convention these features are identified on lunar maps by placing the letter on the side of the crater midpoint that is closest to Eratosthenes.
|A||18.4° N||8.3° W||6 km|
|B||18.7° N||8.7° W||5 km|
|C||16.9° N||12.4° W||5 km|
|D||17.5° N||10.9° W||4 km|
|E||18.0° N||10.9° W||4 km|
|F||17.7° N||9.9° W||4 km|
|H||13.3° N||12.2° W||3 km|
|K||12.9° N||9.2° W||5 km|
|M||14.0° N||13.6° W||4 km|
|Z||13.8° N||14.1° W||1 km|
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