Banded Ridges in Hellas
NASA/JPL/University of Arizona

Banded Ridges in Hellas
ESP_033995_1410  Science Theme: Composition and Photometry
EspañolIcelandic


HICLIP

720p (MP4)  
Listen to the text  

WALLPAPER

800  1024  
1152  1280  
1440  1600  
1920  2048  
2560  2880 

HIFLYER

PDF, 11 x 17 in  

HISLIDES

PowerPoint  
Keynote  
PDF  
Low lying areas in the Hellas region--which is the largest impact basin on Mars--often show complex groups of banded ridges, furrows, and pits. These sorts of bands suggest that the surface material has flowed and twisted viscously like taffy. The orientation of the ridges and groups of ridges would then point in the direction of the flow, called stream lines.

Making this landscape even more complex is when we see that the ridges are sometimes disconnected. They stop abruptly, break up into blocky segments that sometimes appear offset. Such mixed up fragments give an initial sense that parts of the flow have been rafted apart from one another. Alternatively, the entire region may be substantially eroded since the time when the taffy-like ridges actually formed. In that case, the flow may have been far more complex and three dimensional, such that the disconnected portions are actually areas where the flow transitioned up and down relative to the current plane of the eroded surface. In this way we only see a slice through a far more complex series of twists and bends, some of which is still buried beneath the ground.

What this taffy-like material is made of is currently unknown. Hard and soft rocks, as well as ice and ice-rich rocky debris, can deform and flow given time under the force of gravity and the pressures found deep beneath the surface. Afterwards, differential erosion of hard and soft rock or icy materials mixed in bands and layers might give rise to the ridges, furrows and pits which we observe today.

Written by: Mike Mellon (audio by Tre Gibbs)   (9 January 2014)



 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 (623.1 MB)
IRB color: map-projected (336.7 MB)

JP2 EXTRAS
Grayscale: map-projected  (379.5 MB),
non-map  (383.8 MB)
IRB color: map projected  (198.5 MB)
non-map  (371.6 MB)
Merged IRB: map projected  (667.1 MB)
Merged RGB: map-projected  (619.5 MB)
RGB color: non map-projected  (344.3 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:27 October 2013 Local Mars time: 2:58 PM
Latitude (centered):-38.444° Longitude (East):55.534°
Range to target site:259.2 km (162.0 miles)Original image scale range:51.9 cm/pixel (with 2 x 2 binning) so objects ~156 cm across are resolved
Map projected scale:50 cm/pixel and North is upMap projection:Equirectangular
Emission angle:2.3° Phase angle:70.6°
Solar incidence angle:69°, with the Sun about 21° above the horizon Solar longitude:41.3°, Northern Spring
For non-map projected products:
North azimuth:97° Sub-solar azimuth:50.0°
For map-projected products
North azimuth:270°Sub solar azimuth:222.4°

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.