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A wrinkle ridge is a type of feature commonly found on lunar maria. These features are low, sinuous ridges formed on the mare surface that can extend for up to several hundred kilometers. Wrinkle ridges are tectonic features created when the basaltic lava cooled and contracted. They frequently outline ring structures buried within the mare, follow circular patterns outlining the mare, or intersect protruding peaks. They are sometimes called veins due to their resemblance to the veins that protrude from beneath the skin. These are found near craters.
Wrinkle ridges are named with the Latin designation dorsum (plural dorsa). The standard IAU nomenclature uses the names of people to identify wrinkle ridges on the Moon. Thus the Dorsa Burnet are named for Thomas Burnet, and the Dorsum Owen is named after George Owen of Henllys.
Wrinkle ridges can also be found on Mars, for example in Chryse Planitia, on several of the asteroids that have been visited by spacecraft, on Mercury, and certain moons of Jupiter and Saturn. Although several hypotheses have been advanced as causes of wrinkle ridges, today they are generally considered to be of tectonic origin. They involve folding and faulting. If correctly interpreted as thrust faults, where a rupture occurs and one side of the rupture is pushed on top of the other, they are evidence of compressional stress in planetary crust.
Solis Dorsa are an expansive set of parallel wrinkle ridges on Solis Planum on Mars. Viking 1 Oribiter mosaic.
Floor and eroded south wall of the crater Flaugergues on Mars. Arrows point to wrinkle ridges.
Wrinkle ridges in Hesperia Planum, Mars, as seen by Viking The wrinkle ridges trend in different directions, so compressional forces may have changed direction over time.
Trough cutting a wrinkle ridge, as seen by HiRISE under HiWish program Location in the Coprates quadrangle, Mars.
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