Craters and Pit Crater Chains in Chryse Planitia
NASA/JPL/University of Arizona

Craters and Pit Crater Chains in Chryse Planitia
PSP_008641_2105  Science Theme: Fluvial Processes
Spanish 



WALLPAPER

800  1024  
1152  1280  
1440  1600  
1920  2048  
2560  
This image was taken of a region in Chryse Planitia where Tiu, Ares, and Kasei Valles end. This relatively flat region is pockmarked by impact craters large and small.

This image contains the side of one crater that is about 5 kilometers in diameter, several closer to 1 km, and many that are smaller than 100 meters. In the large 5 km crater, layers of rock are exposed in the crater wall. This is not surprising, given that Tiu, Ares and Kasei Valles all probably dumped tremendous amounts of sediments here, and each of the layers may represent sedimentary layers. Rays of ejecta are observed in radiating out from the large crater. There is also a younger small crater about half-way down, on the right side of the image that has dark ejecta rays still preserved on the surface.

Pit crater chains, in contrast, are not formed by impacts, but by the collapse of material into a void. In the center of the image is a pit crater chain along the linear feature. This linear feature is a graben, which is a block that had dropped down between two parallel faults. Pit chains commonly form in grabens, where there is collapse of material into the subsurface void. This is because this is an area of extension, or pulling apart of the crust. Pit crater chains are also observed associated with lava tubes in other locations on Mars. So these holes in the ground are distinctly different from the craters caused by impacts visible in the rest of the image.
Written by: Alix Davatzes   (14 July 2008)

  Click to share this post on Twitter Click to share this post on Facebook Click to share this post on Google+ Click to share this post on Tumblr


 Image Products: All image links are drag & drop for HiView, or click to download
JPEG
Grayscale: map projected  non-map
IRB color: map projected  non-map
Merged IRB: map projected
Merged RGB: map projected
RGB color: non-map projected

JP2 DOWNLOAD
Grayscale: map-projected (925.1 MB)
IRB color: map-projected (474.8 MB)

JP2 EXTRAS
Grayscale: map-projected  (504.4 MB),
non-map  (437.0 MB)
IRB color: map projected  (202.5 MB)
non-map  (425.0 MB)
Merged IRB: map projected  (944.0 MB)
Merged RGB: map-projected  (882.3 MB)
RGB color: non map-projected  (401.9 MB)

ADDITIONAL IMAGE INFORMATION
Grayscale label   Color label
Merged IRB label   Merged RGB label
EDR products

About color products (PDF)
HiView main page

 Observation Toolbox
Acquisition date:30 May 2008 Local Mars time: 3:11 PM
Latitude (centered):30.360° Longitude (East):323.373°
Range to target site:292.6 km (182.9 miles)Original image scale range:58.5 cm/pixel (with 2 x 2 binning) so objects ~176 cm across are resolved
Map projected scale:50 cm/pixel and North is upMap projection:Equirectangular
Emission angle:0.3° Phase angle:42.4°
Solar incidence angle:42°, with the Sun about 48° above the horizon Solar longitude:78.8°, Northern Spring
For non-map projected products:
North azimuth:97° Sub-solar azimuth:10.4°
For map-projected products
North azimuth:270°Sub solar azimuth:184.3°

Context map

Usage Policy
All of the images produced by HiRISE and accessible on this site are within the public domain: there are no restrictions on their usage by anyone in the public, including news or science organizations. We do ask for a credit line where possible: Image: NASA/JPL/University of Arizona
Postscript
For information about NASA and agency programs on the Web, visit: http://www.nasa.gov. NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, Calif., manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems is the prime contractor for the project and built the spacecraft. The HiRISE camera was built by Ball Aerospace and Technology Corporation and is operated by the University of Arizona. The image data were processed using the U.S. Geological Survey’s ISIS3 software.