A lunar Scene Shows a Close-up Sharp View of Copernicus Crater


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Captured on March 23, 2021 from Dark Sky® Alqueva Observatory, in Cumeada village, Portugal, on a very steady night, the close-up view shows a high-resolution sharp view of Copernicus crater. Visible slightly northwest of the center of the Moon’s Earth-facing hemisphere, Copernicus is an impact crater located on the eastern Oceanus Procellarum. With a diameter of 96,1km and a depth of 3.8 km, it may have been created by debris from the breakup of the parent body of asteroid 495 Eulalia, around 800 million years ago. The circular rim has a discernible hexagonal form, with a terraced inner wall and a 30 km wide, sloping rampart that descends nearly a kilometer to the surrounding mare. There are three distinct terraces visible, and arc-shaped landslides due to slumping of the inner wall as the crater debris subsided. Most likely due to its recent formation, the crater floor has not been flooded by lava. The terrain along the bottom is hilly in the upper part, while the other half is relatively smooth. The central peaks separated from each other by valleys, consist of three isolated mountainous rises climbing as high as 1.2 km above the floor. The crater rays spread as far as 800 kilometers across the surrounding mare, overlying rays from the craters Aristarchus and Kepler. The data on this description are based in the data of Lunar Orbiter 5, Terry W. Offield of the U.S. Geological Survey.


PT: Captada em 23 de Março de 2021 a partir do Observatório da Cumeada, no Dark Sky® Alqueva, Portugal, numa noite com a atmosfera muito estável, mostra uma visão nítida em alta resolução da cratera Copernicus. Visível ligeiramente a noroeste do centro do hemisfério da Lua que está voltado para a Terra, Copernicus é uma cratera de impacto localizada ana região Este do Oceanus Procellarum. Com um diâmetro de 96,1 km e uma profundidade de 3,8 km, pode ter sido criada por destroços do asteróide 495 Eulália, há cerca de 800 milhões de anos atrás. As paredes externas circulares têm uma forma hexagonal perceptível, com uma parede interna em forma de terraço e uma muralha inclinada de 30 km de largura que desce quase um quilômetro até o mar circundante. Existem três terraços distintos visíveis e deslizamentos de terra em forma de arco devido à queda da parede interna à medida que os detritos da cratera diminuíram. Muito provavelmente, devido à sua formação recente, o fundo da cratera não foi inundado por lava. O terreno ao longo do fundo é acidentado na parte superior, enquanto a outra metade é relativamente plana. Os picos centrais separados uns dos outros por vales, consistem em três elevações montanhosas isoladas que chegam a 1,2 km acima do solo. Os raios de impacto da cratera estenderam-se até 800 quilômetros ao redor do mar, sobrepondo-se aos raios das crateras Aristarchus e Kepler. Os dados utlizados na pormenorização desta cratera baseiam-se nos dados do Lunar Orbiter 5, e na descrição detalhada do Terry W. Offield do U.S. Geological Survey.


Technical details | Detalhes Técnicos

Camera ASI174MC | Meade UHTC LX200 12″ GPS|  Barlow 4x Televue Powermate | Sum of 200 frames for each panel. Processing on AutoStakkert 3, Registax 6 and Photoshop CC 2021. Cumeada Observatory from Dark Sky® Alqueva Reserve, Reguengos de Monsaraz.

 

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