Time-Lapse Case Study
NASA/JPL/University of Arizona
Time-Lapse Case Study
PSP_005579_0935  Science Theme: Seasonal Processes

This caption is part of a December 2007 AGU presentation "Spring at the South Pole of Mars."

The sequence of events experienced by araneiform (spider-like) terrain at Mars' south pole are investigated in a series of images acquired through spring and summer in the southern hemisphere.

In subimage 1 (taken from PSP_002532_0935) we zoom in on a single "spider." This is a radially organized collection of channels in the surface, covered by a layer of translucent seasonal carbon dioxide ice. The "date" is Ls = 181.1. (Ls is the way we measure time on Mars: at Ls = 180 the sun passes the equator on its way south; at Ls = 270 it reaches its maximum subsolar latitude and summer begins.)

Subimage 2 (PSP_002850_0935) was acquired at Ls = 195.4. Four dust fans have emerged from the spider's channels. Translucent ice is warmed from below, and evaporates below the seasonal ice layer. The gas finds a weak spot and vents to the top of the ice layer above, carrying dust from the surface along. The dust is blown around by the prevailing wind.

Subimage 3 (PSP_002942_0935) was acquired at Ls = 199.6. Dust is getting trapped in the channels.

Subimage 4 (PSP_003496_0935), acquired at Ls = 226, shows that the wind direction has changed, the existing fans have lengthened, and there are numerous new fans coming from the channels as the overlying ice layer thins.

Subimage 5 (PSP_003641_0935) was taken at Ls = 233.1, when most of the surface frost is gone. The channels are bright because the sun is shining more directly on the walls. A thin lane of dark dust can be seen on the bottom of the largest channels.

Subimage 6 (PSP_005579_0935) was taken at Ls = 325.4, well into southern summer. All seasonal frost is gone. It is clear that channels are carved into the surface, not the seasonal ice. Fans have disappeared in the sense that they no longer contrast with the very surface material that they came from in the first place. The surface material is water-ice cemented dirt covered with a layer ~5 cm deep of desiccated silt-sized dust, which is redistributed every season in this process of fan creation and deposition. Written by: Candy Hansen  (12 December 2007)
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Acquisition date
05 October 2007

Local Mars time:

Latitude (centered)

Longitude (East)

Range to target site
247.9 km (154.9 miles)

Original image scale range
24.8 cm/pixel (with 1 x 1 binning) so objects ~74 cm across are resolved

Map projected scale
25 cm/pixel

Map projection

Emission angle:

Phase angle:

Solar incidence angle
75°, with the Sun about 15° above the horizon

Solar longitude
325.4°, Northern Winter

For non-map projected images
North azimuth:  127°
Sub-solar azimuth:  55.6°
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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.