Variable features on Mars: Preliminary mariner 9 television results

Sagan, Carl; Veverka, J.; Fox, Paul L.; Dubisch, Russell; Lederberg, Joshua; Levinthal, Elliott C.; Quam, Lynn H.; Tucker, Robert B.; Pollack, James B.; Smith, B. A.

doi:10.1016/0019-1035(72)90005-x

Cited by 157 publications

(80 citation statements)

References 14 publications

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“…As spacecraft began to explore the planet, a geological interpretation emerged that invoked eolian erosion and deposition of bright dust to explain the albedo patterns and observed changes [Rea, 1964;Sagan and Pollack, 1969]. The arrival of Mariner 9 during a major global dust obscuration event in November 1971, followed by the gradual clearing of the atmosphere and observation of rapid changes in surface albedo patterns [Sagan et al, 1972[Sagan et al, , 1973 …”

Section: Introductionmentioning

confidence: 99%

New views of Mars eolian activity, materials, and surface properties: Three vignettes from the Mars Global Surveyor Mars Orbiter Camera

Edgett¹,

Malin²

2000

J. Geophys. Res.

142

118

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Section: Introductionmentioning

confidence: 99%

New views of Mars eolian activity, materials, and surface properties: Three vignettes from the Mars Global Surveyor Mars Orbiter Camera

Edgett¹,

Malin²

2000

J. Geophys. Res.

142

118

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“…Sand dunes have been found on Mars for the first time in Mariner 9 images of the Proctor Crater, within the southern highlands of Mars (McCauley et al 1972;Sagan et al 1972). Since then, other Missions sent to Mars provided us with thousands of images which revealed a rich diversity of dune shapes including barchans, transverse dunes, and also linear and star dunes (Edgett and Blumberg 1994).…”

Section: Discussionmentioning

confidence: 99%

Vegetation and Induration as Sand Dunes Stabilizators

Herrmann

Durán²,

Parteli

et al. 2008

Journal of Coastal Research

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Sand dunes are found in a wide variety of shapes in deserts and coasts, and also on the planet Mars. The basic mechanisms of dune formation could be incorporated into a continuum saltation model, which successfully reproduced the shape of the barchan dunes and has been also applied to calculate interaction of barchans in a field. We have recently extended our dune model to investigate other dune shapes observed in nature. Here, we present the first numerical simulation of the transformation of barchan dunes, under influence of vegetation, into parabolic dunes, which appear frequently on coasts. Further, we apply our model to reproduce the shape of barchan dunes observed on Mars, and we find that an interesting property related to the martian saltation is relevant to predict the scale of dunes on Mars. Our model could also reproduce unusual dune shapes of the Martian north polar region, like rounded barchans and elongated linear dunes. Our results support the hypothesis that these dunes are indurated.

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“…Chaotic terrain covers more than 1% of the Martian surface. Indeed several of the major sinuous channels are discovered emanating from chaotic terrain, and there Sagan et al, 1972). This permits aeolian transp;;rt of macrobial as well as microbial dispersules (cf., e.g., fern spores or pine tree pollen).…”

Section: Microbes and Macrobesmentioning

confidence: 99%