Abstract
Abstract A classification of Martian wind streaks has been developed to assist in investigations of eolian transport and related meteorological phenomena on Mars. Streaks can be grouped by their albedo contrast with their surroundings and by the presence of either topographic obstacles or sediment deposits at their points of origin. The vast majority of wind streaks can be included in three categories. (1) Bright streaks with no source deposit: interpreted to be formed by preferential deposition of dust from suspension. (2) Dark streaks with no source deposit: interpreted to be formed by preferential erosion of bright dust and its removal in suspension. (3) Dark streaks associated with deposits of sediment: interpreted to be formed by deposition of dark material moved by saltation. The orientations of the different streak types are distinctive and reflect both global flow patterns and slope-controlled winds. The wind directions derived from streaks and the geographical distribution of the features show a strong north-south asymmetry—consistent with the fact that perihelion (and hence maximum wind activity) occurs near southern summer solstice.
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