Escalante Crater Wall, as seen by HiRISE. Picture on left is enlargement of the one on right. Scale bar is long.
|Eponym||Mexican astronomer F. Escalante|
Escalante Crater is an impact crater in the Amenthes quadrangle of Mars. It is located at 0.2° N and 244.7° W. It is 79.3 km (49.3 mi) in diameter, and was named after Mexican astronomer (c. 1930) F. Escalante.
CTX camera (on Mars Reconnaissance Orbiter) image of Escalante Crater. Dunes are visible near the bottom of the image.
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. If one measures the diameter of a crater, the original depth can be estimated with various ratios. Because of this relationship, researchers have found that many Martian craters contain a great deal of material; much of it is believed to be ice deposited when the climate was different. Sometimes craters expose layers that were buried. Rocks from deep underground are tossed onto the surface. Hence, craters can show us what lies deep under the surface. A pedestal crater is a crater with its ejecta sitting above the surrounding terrain and thereby forming a raised platform. This type of crater forms when an impact crater ejects material which forms an erosion resistant layer, thus protecting the immediate area from erosion. As a result of this hard covering, the crater and its ejecta become elevated when erosion removes the softer material that lies beyond the ejecta. Some pedestals have been accurately measured to be hundreds of meters above the surrounding area. This means that hundreds of meters of material were eroded away. Pedestal craters were first observed during the Mariner missions.
Why are Craters important?
The density of impact craters is used to determine the surface ages of Mars and other solar system bodies. The older the surface, the more craters present. Crater shapes can reveal the presence of ground ice.
The area around craters may be rich in minerals. On Mars, heat from the impact melts ice in the ground. Water from the melting ice dissolves minerals, and then deposits them in cracks or faults that were produced with the impact. This process, called hydrothermal alteration, is a major way in which ore deposits are produced. The area around Martian craters may be rich in useful ores for the future colonization of Mars. Studies on the earth have documented that cracks are produced and that secondary minerals veins are deposited in the cracks. Images from satellites orbiting Mars have detected cracks near impact craters. Great amounts of heat are produced during impacts. The area around a large impact may take hundreds of thousands of years to cool. Many craters once contained lakes. Because some crater floors show deltas, we know that water had to be present for some time. Dozens of deltas have been spotted on Mars. Deltas form when sediment is washed in from a stream entering a quiet body of water. It takes a bit of time to form a delta, so the presence of a delta is exciting; it means water was there for a time, maybe for many years. Primitive organisms may have developed in such lakes; hence, some craters may be prime targets for the search for evidence of life on the Red Planet.
- Impact crater
- List of craters on Mars
- Water on Mars
- Climate of Mars
- Deuteronilus Mensae
- Fretted terrain
- Glaciers on Mars
- Lobate debris apron
- Protonilus Mensae
- Ore genesis
- Ore resources on Mars
- Hydrothermal circulation
- Gazetteer of Planetary Nomenclature Feature Information
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