Valles Marineris. Mars Reconnaissance Orbiter (MRO) image showing layers and exposed bedrock along a cliff in west Candor Chasma, part of the extensiv

RMID:2ACYA6A

Preview

Buy the print

Image details

Contributor:

Science Photo Library / Alamy Stock Photo

Image ID:

2ACYA6A

File size:

25.1 MB (1.1 MB Compressed download)

Releases:

Model - no | Property - noDo I need a release?

Dimensions:

3749 x 2343 px | 31.7 x 19.8 cm | 12.5 x 7.8 inches | 300dpi

Date taken:

16 October 2014

Photographer:

NASA/SCIENCE PHOTO LIBRARY

More information:

Valles Marineris. Mars Reconnaissance Orbiter (MRO) image showing layers and exposed bedrock along a cliff in west Candor Chasma, part of the extensive Valles Marineris canyon system on the surface of Mars. Imaged by the MRO's HiRISE (High Resolution Imaging Science Experiment) camera.

Search stock photos by tags

Similar stock images

RF2K6A83T–A colorful landslide in Eos Chasma in the southern part of the Valles Marineris on the planet Mars.

RF2M16B4A–The planet Mars

RF2K6A87B–View of Aram Chaos, an ancient impact crater that lies in the Southern Highlands of Mars.

RMT8075B–Mars Before and After Dust Storm

RM2WBMYY8–Candor Chasma in central Valles Marineris is filled with light-toned layered deposits thought to be sandstones, perhaps formed in an ancient wet and potentially habitable environment. The CRISM instrument on MRO has acquired thousands high-resolution spectral images across Mars, often with simultaneous coverage by HiRISE, but sometimes, for a variety of reasons, without HiRISE coverage. We are now trying to complete coordinated coverage over such locations, to enable geologic interpretations based on both the compositional information of CRISM and the high-resolution imaging of HiRISE.

RF2M4EMG5–The planet Mars

RM2K5D50G–This image shows a crater on the floor of Eos Chasma, part of the Valles Marineris canyon system. Craters on Mars are useful for geologists because they provide cross-sections into the subsurface. The south wall of this crater shows evidence of several different types of rock, with diverse colors. In the black and white parts of the image, it appears that there are two types of rock one relatively light and one dark. However, in the 1.1 kilometer-wide color swath we can see that the dark rocks are more complicated, as some have a greenish tint and others are purple. Note that these are not the

RM2K5D136–Massive deposits of sediments rich in hydrated sulfates are found in central Valles Marineris. Such deposits on Earth are soft and easily eroded, and that appears to be true on Mars as well. There are large gullies and sediment fans along the steepest slopes. Elsewhere on Mars, such slopes are actively eroding in before-and-after HiRISE images, so this would be a good location to observe again in a future year. Linear gaps in data coverage on the bright sun-facing slopes are locations where the image data is saturated.

RM2T2BB9T–. Diverse Minerals in Coprates Chasma. This image shows the southern wall of Coprates Chasma, in the equatorial canyon system of Valles Marineris. While much of the lower slopes are covered by sand, exposed bedrock is clearly visible in the upper canyon walls. In an enhanced color image, the varying colors – shades of white, cyan, and purple – are suggestive of multiple minerals being present within the bedrock, indicating a complicated geologic history, possibly involving alteration by water. (In this cutout, north is down.)

RM2T2BBAJ–. Light-Toned Materials along the Floor and Walls of Ius Chasma. Many of the Valles Marineris canyons, called chasmata, have kilometer-high, light-toned layered mounds made up of sulfate materials. Ius Chasma, near the western end of Valles Marineris, is an exception. The light-toned deposits here are thinner and occur along both the floor and walls, as we see in this HiRISE image. Additionally, the sulfates are mixed with other minerals like clays and hydrated silica. Scientists are trying to use the combination of mineralogy, morphology, and stratigraphy to understand how the deposits formed

RM2K5D1CB–Sediments rich in hydrated sulfates may have filled central Valles Marineris, but debates persist as to how these deposits grew or formed. If they formed from deposition in a deep lake then the layers should be nearly horizontal. If the layers formed from airfall deposits such as volcanic pyroclastics or windblown dust, then the layers should drape over the pre-existing topography. Another possibility is that the layers were deformed by slumping. Stereo topographic data can be used to test these hypotheses. The cutout shows an area at full resolution. There are no detectable color variations w

Valles Marineris. Mars Reconnaissance Orbiter (MRO) image showing layers and exposed bedrock along a cliff in west Candor Chasma, part of the extensiv

Image details

Search stock photos by tags

Get great features with your free account

Get inspired for your next project!