Wrinkle ridge in Oceanus Procellarum
November 30, 2012
Just to the north of the WAC context image, there is a small wrinkle ridge ring (not nearly as large as the one in Mare Crisium). This wrinkle ridge ring formed when the compressive stresses creating the wrinkle ridge were changed by the presence of a buried crater. Tectonic features are influenced by regional, large-scale stresses (many 100s of km) and localized, smaller-scale stresses (10s of km). The presence of long wrinkle ridges in the mare are primarily the result of the regional stresses, probably caused by the weight of many layers of extruded basalts. The formation of tectonic features can also be influenced by local stresses, which may result from the presence of a particular geologic feature such as a buried crater or a hill. When features such as these exist, their localized stresses are greater than the large-scale regional stresses. This change in dominating stress field explains how a wrinkle ridge ring forms. How many boulder fields can you find on the wrinkle ridge in the full LROC NAC frame? LROC WAC M117881131M context image of wrinkle ridges in southwestern Oceanus Procellarum. Arrow points at the portion of wrinkle ridge visible in today's Featured Image. Scene is ~82 km across [NASA/GSFC/Arizona State University].