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  • 21 Aug, 2019

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File:Ius Chasma, Valles Marineris, Mars.jpg

The outcrops contain interchanging layers of dark and bright rocks. The layered deposits consist of dark basalt lava flows and bright sedimentary layers. The sediments are likely to be from atmospheric dust, sand or alluvium from an ancient water source. The layers are visible on the gentle slopes above the canyon floor, in pitted areas, and in small mesa buttes. The floor of the canyon is littered with megaripples that are aligned in a north-south direction.

Ius Chasma is believed to have been shaped by a process called sapping when water seeped from the layers of the cliffs and evaporated before it reached the canyon floor. Ius Chasma also has several structural features such as east trending normal faults and grabens that deformed the canyons. Recent geomorphological events include avalanches and minor sapping from gullies that continued to erode the canyon walls.
Date Source NASA website; description,[1] high resolution image.[2] Author NASA/JPL-Caltech/Univ. of Arizona

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Public domain This file is in the public domain in the United States because it was solely created by NASA. NASA copyright policy states that "NASA material is not protected by copyright unless noted". (See Template:PD-USGov, NASA copyright policy page or JPL Image Use Policy.)
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22 September 2008

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current15:58, 5 October 2008Thumbnail for version as of 15:58, 5 October 20082,560 × 1,920 (793 KB)Elipongo{{Information |Description={{en|1=The Red Planet is home to Valles Marineris, the solar system's largest canyon. Within this canyon lies Ius Chasma. This image, which spans the floor of its southern trench,m was taken by the Mars Reconnaissance Orbiter. T

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