Coordinated MER Spirit and MRO HiRISE Imaging Campaign
NASA/JPL/University of Arizona
Coordinated MER Spirit and MRO HiRISE Imaging Campaign
ESP_013499_1650  Science Theme: Future Exploration/Landing Sites
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One of the science objectives of this observation was to try to capture the same dust devil in both cameras simultaneously by coordinated HiRISE and MER Spirit observations.

Surprisingly few dust plumes and dust devil tracks have been observed by HiRISE in Gusev Crater, in comparison to the number of dust devils seen by the rover. Obtaining both ground-based and orbital imagery will allow scientists to better understand the formation, physical properties, and behavior of the dust devils at the MER Spirit landing site.

During these coordinated observations, Spirit observed several small dust devils and a large dust devil in the flat plains northwest of its current position on the western scarp of a polygonal feature commonly called Home Plate. On the other hand, the HiRISE camera did not detect an active dust devil nor the track that dust devils often leave behind. However, a dust devil plume was captured east of Columbia Hills that was about 17 meters in diameter! The top “L-curve” is the track left behind, and the bottom “L-curve” is the shadow of the plume. With changing winds, the dust devil is moving in a direction different than when it formed. It may be that only the largest of the Gusev Crater dust devils can be easily seen by HiRISE.

Ground-based (Mars Exploration Rover) MER and orbital MRO (Mars Reconnaissance Orbiter) HiRISE observations indicate that the low albedo zone in Gusev Crater is currently an active area for the formation of dust devils.

Dust devils are convecting warm-core vortices that form when hot surface air rises and is replaced by the radial inflow of surrounding cool air. This rising vertical column of swirling warm air creates a low pressure core. The low pressure core acts like a vacuum that picks up fine particles that mantle the surface and exposes the dark basaltic substrate in a narrow track.

Subimage credit: Devin Waller, Arizona State University (for Spirit coordination).

Written by: Circe Verba  (2 September 2009)
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Acquisition date
13 June 2009

Local Mars time:

Latitude (centered)

Longitude (East)

Range to target site
268.8 km (168.0 miles)

Original image scale range
26.9 cm/pixel (with 1 x 1 binning) so objects ~81 cm across are resolved

Map projected scale
25 cm/pixel and North is up

Map projection

Emission angle:

Phase angle:

Solar incidence angle
39°, with the Sun about 51° above the horizon

Solar longitude
284.3°, Northern Winter

For non-map projected images
North azimuth:  97°
Sub-solar azimuth:  343.9°
Black and white
map projected  non-map

IRB color
map projected  non-map

Merged IRB
map projected

Merged RGB
map projected

RGB color
non-map projected

Black and white
map-projected   (1062MB)

IRB color
map-projected   (423MB)

Black and white
map-projected  (497MB)
non-map           (595MB)

IRB color
map projected  (197MB)
non-map           (466MB)

Merged IRB
map projected  (258MB)

Merged RGB
map-projected  (253MB)

RGB color
non map           (487MB)
B&W label
Color label
Merged IRB label
Merged RGB label
EDR products

IRB: infrared-red-blue
RGB: red-green-blue
About color products (PDF)

Black & white is 5 km across; enhanced color about 1 km
For scale, use JPEG/JP2 black & white map-projected images

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:
NASA/JPL/University of Arizona

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. The HiRISE camera was built by Ball Aerospace and Technology Corporation and is operated by the University of Arizona.