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Record Details

Record 82 of 187
Stars and linear dunes on Mars
External Online Source: doi:10.1006/icar.1994.1197
Author and Affiliation:
Edgett, Kenneth S.(Arizona State Univ., Tempe, AZ, United States)
Blumberg, Dan G.(Arizona State Univ., Tempe, AZ, United States)
Abstract: A field containing 11 star and incipient star dunes occurs on Mars at 8.8 deg S, 270.9 deg W. Examples of linear dunes are found in a crater at 59.4 deg S, 343 deg W. While rare, dune varieties that form in bi- and multidirectional wind regimes are not absent from the surface of Mars. The occurence of both of these dune fields offers new insight into the nature of martian wind conditions and sand supply. The linear dunes appears to have formed through modification of a formerly transverse aeolian deposit, suggesting a relatively recent change in local wind direction. The 11 dunes in the star dune locality show a progressive change from barchan to star form as each successive dune has traveled up into a valley, into a more complex wind regime. The star dunes corroborate the model of N. Lancaster (1989), for the formation of star dunes by projection of transverse dunes into a complex, topographically influenced wind regime. The star dunes have dark streaks emanating from them, providing evidence that the dunes were active at or near the time the relevant image was obtained by the Viking 1 orbiter in 1978. The star and linear dunes described here are located in different regions on the martian surface. Unlike most star and linear dunes on Earth, both martian examples are isolated occurrences; neither is part of a major sand sea. Previously published Mars general circulation model results suggest that the region in which the linear dune field occurs should be a bimodal wind regime, while the region in which the star dunes occur should be unimodal. The star dunes are probably the result of localized complication of the wind regime owing to topographic confinement of the dunes. Local topographic influence on wind regime is also evident in the linear dune field, as there are transverse dunes in close proximity to the linear dunes, and their occurrence is best explained by funneling of wind through a topographic gap in the upwind crater wall.
Publication Date: Dec 01, 1994
Document ID:
19950053527
(Acquired Dec 28, 1995)
Accession Number: 95A85126
Subject Category: LUNAR AND PLANETARY EXPLORATION
Document Type: Journal Article
Publication Information: Icarus (ISSN 0019-1035); 112; 2; p. 448-464
Publisher Information: United States
Financial Sponsor: NASA; United States
Organization Source: NASA; Washington, DC, United States
Description: 17p; In English
Distribution Limits: Unclassified; Publicly available; Unlimited
Rights: Copyright
NASA Terms: CRATERS; DUNES; MARS (PLANET); WIND EFFECTS; ALBEDO; ATMOSPHERIC MODELS; MORPHOLOGY; TOPOGRAPHY; WIND DIRECTION
Imprint And Other Notes: Icarus vol. 112, no. 2 p. 448-464 December 1994
Miscellaneous Notes: Research sponsored by NASA
Availability Source: Other Sources
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