File:Ablagerungen von dunklem Staub und Sand im Krater Huygens (48758539016).jpeg

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Deutsch: Bei 55 Grad östlicher Länge und 14 Grad südlicher Breite ist in der großen HRSC-Aufnahme der 465 Kilometer große Krater Huygens zu erkennen, benannt nach dem holländischen Astronomen Christiaan Huygens (1629-1695). Wie auch der Krater Cassini ist das Huygens-Becken sehr alt – vermutlich vier Milliarden Jahre oder älter – und bereits stark von der Erosion eingeebnet. Einschlagsstrukturen dieser Größe haben durch die beim Impakt zurückfedernde Kruste des Planeten neben dem eigentlichen Kraterrand im Inneren einen oder mehrere Ringe. Beim Krater Cassini ist dieser Ring in der Topographie nicht mehr zu erkennen, bei Huygens hingegen schon – dunkler, vom Wind ins Innere des Kraters verfrachteter Sand lässt die Struktur des inneren Ringes hervortreten. Wind ist derjenige Prozess auf dem Mars, der gegenwärtig die größten Veränderungen der Oberfläche bewirkt. So lässt sich heute vielerorts die Verlagerung von dunklen Sanden durch Wind beobachten. Während diese vulkanisch entstandenen Sande in Senken, wie beispielsweise Einschlagskratern, mächtige Dünenfelder bilden, sind sie auf größeren Flächen oft als ausgedehnte Sandlagen abgelagert, die große Teile des Planeten dunkel erscheinen lassen. Verlagerung von Dünen kann man schon in Zeitskalen von ein bis zwei Jahren mit hochauflösenden Bilddaten beobachten.

Mehr dazu: www.dlr.de/content/de/artikel/news/2019/03/20190919_mars-...

Credit: ESA/DLR/FU Berlin, CC BY-SA 3.0
English: At longitude 55 degrees east and latitude 14 degrees south, the large HRSC image shows the 465-kilometer-wide Huygens Crater, named after the Dutch astronomer Christiaan Huygens (1629-1695). Like the Cassini crater, the Huygens Basin is very old—probably four billion years or more—and already heavily eroded. Impact structures of this size have one or more rings in the interior next to the actual rim of the crater due to the crust of the planet springing back during the impact. In the case of the Cassini crater, this ring can no longer be recognized in the topography, but it can be seen in the case of Huygens - dark sand transported into the interior of the crater by the wind makes the structure of the inner ring stand out. Wind is the process on Mars that is currently causing the greatest surface changes. The shifting of dark sands by wind can be observed in many places today. While these volcanic sands form massive dune fields in depressions such as impact craters, over larger areas they are often deposited as extensive sand layers that make large parts of the planet appear dark. Shifting of dunes can already be observed on a time scale of one to two years with high-resolution image data. More on this: www.dlr.de/content/de/artikel/news/2019/03/20190919_mars-... Credit: ESA/DLR/FU Berlin, CC BY-SA 3.0
Date Taken on 19 September 2019, 11:39:30
Source Ablagerungen von dunklem Staub und Sand im Krater Huygens
Author DLR_de
Flickr set
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Mars Express
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roterplanet; marsexpress; hellas; mars; raumfahrt; huygens; stereokamera; hrsc; planetenforschung; kamera; krater; cassini

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This image was originally posted to Flickr by DLR_de at https://flickr.com/photos/48213136@N06/48758539016. It was reviewed on 13 February 2023 by FlickreviewR 2 and was confirmed to be licensed under the terms of the cc-by-sa-2.0.

13 February 2023

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w:en:Creative Commons
attribution share alike
This file is licensed under the Creative Commons Attribution-ShareAlike 3.0 IGO license.
Attribution: ESA/DLR/FU Berlin, CC BY-SA IGO 3.0
You are free:
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Under the following conditions:
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