This image from Magellan's 383rd orbit of Venus shows about half of an unnamed 47 kilometers diameter (28 miles) impact crater; it is the second largest of three similar craters closely grouped in a region of radar-dark (smooth) plains between Lavinia Planitia and Guinevere Planitia. The crater, located at latitude 26.4 degrees S. and longitude 337.3 degrees, was previously seen in Earth-based radar images acquired at the Arecibo radar observatory in Puerto Rico. The crater has many characteristics typical of meteorite impact craters, including a central peak, deposits of hummocky or hilly material immediately surrounding the crater's rim, and smoother more patchy deposits that extend further from the crater rim. Some of the hummocky ejecta appears to extend for some distance along the major lobes formed by the outer ejecta. This radial distribution of the hummocky ejecta may be a consequence of the way the material was thrown from the crater and moved through the atmosphere and along the surface. far-flung ejecta, are also present near the most distal parts of the outer ejecta deposits. The radar-bright ejecta and inner wall of this crater indicate that it is fresh and not noticeably degraded. The resolution of this image is about 150 meters (450 feet); north is to the top. The Magellan radar was illuminating the surface from left to right in this image.The crater's central peak, and flat floor are also common to many other impact structures; the latter probably formed by the ponding of lava flows on the crater's floor. Secondary impact craters formed by
