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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, as well as on several of the asteroids that have been visited by spacecraft, as well as Mercury, and a couple of moons of Jupiter and Saturn. Although several hypotheses have been advanced as causes of Martian wrinkle ridges, today they are generally considered to be of tectonic origin. They involve folding and faulting.〔Kieffer, H, B. Jakosky, C. Snyder, M. Matthews (eds.). 1992. Mars. University of Arizona Press.〕 Wikiflaugergues.jpg|Part of floor and eroded south wall of Flaugergues Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter). Arrows point to wrinkle ridges. ==See also== *List of features on the Moon *Planetary nomenclature 抄文引用元・出典: フリー百科事典『 ウィキペディア（Wikipedia）』 ■ウィキペディアで「Wrinkle ridge」の詳細全文を読む スポンサード リンク
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