Wind streaks: geological and botanical effects on surface albedo contrast

Zimbelman, J. R.; Williams, S. H.

doi:10.1016/0169-555x(95)00098-p

Cited by 13 publications

(10 citation statements)

References 27 publications

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“…Inferences made from analysis of aerial photographs of terrestrial wind streaks are usually found to lack important, sometimes unexpected, detail when investigated in the field. For example, the aerial visibility of a wind streak at Sleeping Beauty Mountain, California, was found to be modulated by the presence of annual changes in grass cover, and whether a particular grass grew on or off the streak was dependent upon the sediment and regolith properties of the streak and adjacent surface materials [ Zimbelman and Williams , 1996]. Despite the limitations of photogeology, there are specific features that can be sought and examined in MOC images that provide clues to genesis of Martian wind streaks.…”

Section: West Arabia Streak Genesis and Tests With Mocmentioning

confidence: 99%

Low‐albedo surfaces and eolian sediment: Mars Orbiter Camera views of western Arabia Terra craters and wind streaks

Edgett

2002

J.‐Geophys.‐Res.

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[1] High spatial resolution (1.5 to 6 m/pixel) Mars Global Surveyor Mars Orbiter Camera images obtained September 1997 to June 2001 show that each of the large, dark wind streaks of western Arabia Terra originate at a barchan dune field on a crater floor. The streaks consist of a relatively thin (<1 m) coating of sediment deflated from the dune fields and their vicinity. In most cases, this sediment drapes over a previous mantle that more thickly covers nearly all of western Arabia Terra. No concurrent eolian bedforms are found within the dark streaks, nor do any dunes climb up crater walls to deliver sand via saltation to the streaks. The relations between dunes, wind streak, and subjacent terrain imply that dark-toned grains finer than those that comprise the dunes are lifted into suspension and carried out of the craters to be deposited on the adjacent terrain. Previous eolian physics and thermal inertia studies suggest that, under modern Martian conditions, such grains likely include silt (3.9-62.5 mm), very fine sand (62.5-125 mm), and possibly fine sand (to $210 mm). The streaks change in terms of extent, relative albedo, and surface pattern over periods measured in years; however, through June 2001, very little evidence for recent eolian activity (dust plumes, storms, dune movement) was observed.

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Section: West Arabia Streak Genesis and Tests With Mocmentioning

confidence: 99%

Low‐albedo surfaces and eolian sediment: Mars Orbiter Camera views of western Arabia Terra craters and wind streaks

Edgett

2002

J.‐Geophys.‐Res.

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“…1-3) and Earth (Fig. 4), but they are significantly more abundant on Mars, where they comprise widespread young aeolian features that typically occur in the lee of impact craters (Thomas et al, 1981;Lee, 1984) and have high length-width ratios (Greeley et al, 1974a,b;Maxwell and El-Baz, 1982;Greeley, 1986;Greeley et al, 1989;Zimbelman and Williams, 1996). Based on the inferred morphogenesis of Martian wind streaks, Thomas et al (1981) classified them into three subsets, those produced: (1) by wind erosion and removal of surficial sediments from the lee of topographic obstacles; (2) from the preservation of surficial sediments located in the lee of topographic obstacles; and (3) by the aeolian deflation of sediments, typically intra-crater dune fields, and subsequent deposition downwind of the source.…”

Section: Introductionmentioning

confidence: 95%

“…Wind-tunnel modeling and fieldwork studies of wind streaks (Greeley et al, 1974a,b;Maxwell and El-Baz, 1982;Greeley, 1986;Greeley et al, 1989;Zimbelman and Williams, 1996) indicate that the formation of wind streaks involves three modes of sediment transport-saltation, traction, and suspension-and a range of particle sizes from clay through granules (Edgett, 2002).…”

Section: Introductionmentioning

confidence: 96%

“…Terrestrial wind streaks have been studied at several locations (Maxwell and El-Baz, 1982;Greeley and Iversen, 1985;Zimbelman, 1986;Greeley et al, 1989) and appear to have a variety of characteristics and origins (Zimbelman, 1986;Greeley et al, 1989;Zimbelman and Williams, 1996). Wind-tunnel modeling and fieldwork studies of wind streaks (Greeley et al, 1974a,b;Maxwell and El-Baz, 1982;Greeley, 1986;Greeley et al, 1989;Zimbelman and Williams, 1996) indicate that the formation of wind streaks involves three modes of sediment transport-saltation, traction, and suspension-and a range of particle sizes from clay through granules (Edgett, 2002).…”

Section: Introductionmentioning

confidence: 99%

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The sedimentology and dynamics of crater-affiliated wind streaks in western Arabia Terra, Mars and Patagonia, Argentina

et al. 2010

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“…One of the most studied sites as an analogue to the Martian wind streaks is Amboy, California [ Greeley and Iversen , ; Greeley and Iversen , ; Greeley and Iversen , ; Zimbelman and Williams , ]. Kienenberger and Greeley [] conducted field work on the distribution of windblown sediments in the Amboy lava field.…”

Section: Discussionmentioning

confidence: 99%

Earth aeolian wind streaks: Comparison to wind data from model and stations

2017

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Wind streak is a collective term for a variety of aeolian features that display distinctive albedo surface patterns. Wind streaks have been used to map near‐surface winds and to estimate atmospheric circulation patterns on Mars and Venus. However, because wind streaks have been studied mostly on Mars and Venus, much of the knowledge regarding the mechanism and time frame of their formation and their relationship to the atmospheric circulation cannot be verified. This study aims to validate previous studies' results by a comparison of real and modeled wind data with wind streak orientations as measured from remote‐sensing images. Orientations of Earth wind streaks were statistically correlated to resultant drift direction (RDD) values calculated from reanalysis and wind data from 621 weather stations. The results showed good agreement between wind streak orientations and reanalysis RDD (r = 0.78). A moderate correlation was found between the wind streak orientations and the weather station data (r = 0.47); a similar trend was revealed on a regional scale when the analysis was performed by continent, with r ranging from 0.641 in North America to 0.922 in Antarctica. At sites where wind streak orientations did not correspond to the RDDs (i.e., a difference of 45°), seasonal and diurnal variations in the wind flow were found to be responsible for deviation from the global pattern. The study thus confirms that Earth wind streaks were formed by the present wind regime and they are indeed indicative of the long‐term prevailing wind direction on global and regional scales.

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Wind streaks: geological and botanical effects on surface albedo contrast

Cited by 13 publications

References 27 publications

Low‐albedo surfaces and eolian sediment: Mars Orbiter Camera views of western Arabia Terra craters and wind streaks

Low‐albedo surfaces and eolian sediment: Mars Orbiter Camera views of western Arabia Terra craters and wind streaks

The sedimentology and dynamics of crater-affiliated wind streaks in western Arabia Terra, Mars and Patagonia, Argentina

Earth aeolian wind streaks: Comparison to wind data from model and stations

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