Noachis Quadrangle - Craters

Craters

Impact craters generally have a rim with ejecta around them, in contrast volcanic craters usually do not have a rim or ejecta deposits. As craters get larger (greater than 10 km in diameter) they usually have a central peak. The peak is caused by a rebound of the crater floor following the impact. Sometimes craters will display layers. Craters can show us what lies deep under the surface.

• Maunder Crater, as seen by HiRISE. The overhang is part of the degraded south (toward bottom) wall of crater. The scale bar is 500 meters long.

• Asimov Crater, as seen by HiRISE. Bottom of picture shows southeastern wall of crater. Top of picture is edge of mound that fills most of the crater.

• Gullies on mound in Asimov Crater, as seen by HiRISE.

• Layers in west slope of Asimov Crater, as seen by HiRISE.

• Close-up of layers in west slope of Asimov Crater. Shadows show the overhang. Some of the layers are much more resistant to erosion, so they stick out. Image from HiRISE.

• East Slope of Central Pit in Asimov Crater, as seen by HiRISE. Click on image to see more details of the many gullies.

• Kaiser Crater (large crater in upper part of image)context for THEMIS image.

• Detail of south wall of Kaiser Crater, as seen by THEMIS. Top of image shows part of a dune field.

• Rabe Crater Floor, as seen by HiRISE. Click on image to see layers. Dark sand that made the dunes was probably blown in from elsewhere.

• Crater that was buried in another age and is now being exposed by erosion, as seen by the Mars Global Surveyor, under the MOC Public Targeting Program.

• Floor of crater in Noachis quadrangle, as seen by HiRISE under HiWish program.