Arandas is a crater in the Mare Acidalium quadrangle of Mars, located 42.77° North and 15.17° West. It is 24.76 km (15.39 mi) in diameter and is named after the town of Arandas in Mexico.[1]
 Arandas crater, as seen by HiRISE. Click on image for a better view of North and South Walls, as well as central hills. Scale bar is 1000 meters long. | |
| Planet | Mars |
|---|---|
| Coordinates | 42°46′N 15°10′W / 42.77°N 15.17°W |
| Quadrangle | Mare Acidalium |
| Diameter | 24.76 km (15.39 mi) |
| Eponym | The town of Arandas in Mexico |
Gullies are visible in Arandas. On the basis of their form, aspects, positions, and location amongst an apparent interaction with features thought to be rich in water ice, many researchers believed that the processes carving the gullies involve liquid water. However, this remains a topic of active research. As soon as gullies were discovered,[2] researchers began to image many gullies over and over, looking for possible changes. By 2006, some changes were found.[3] Later, with further analysis it was determined that the changes could have occurred by dry granular flows rather than being driven by flowing water.[4][5][6] With continued observations many more changes were found in Gasa Crater and others.[7] As further observations have been made, still more changes have been noted; since the changes occur in the winter and spring, experts tend to believe that gullies were formed from dry ice. Before-and-after images demonstrated the timing of this activity coincided with seasonal carbon-dioxide frost and temperatures that would not have allowed for liquid water. When dry ice frost changes to a gas, it may lubricate dry material to flow, especially on steep slopes.[8][9][10]
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MOLA map showing Arandas crater and other nearby craters. Color indicates elevation. -
Arandas crater, as seen by CTX camera (on MRO). -
Gullies in Arandas, as seen by CTX camera. Note: this is an enlargement of the previous photo. -
Gullies in Arandas, as seen by HiRISE under HiWish program.
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 (6.2 mi) in diameter) they usually have a central peak.[11] The peak is caused by a rebound of the crater floor following the impact.[12] Sometimes craters expose layers that were buried. Rocks from deep underground are tossed onto the surface. Hence, craters can expose what lies deep under the surface.
See also
editReferences
edit- ^ "Arandas". planetarynames.wr.usgs.gov. International Astronomical Union. Retrieved 3 July 2015.
- ^ Malin, M., Edgett, K. 2000. "Evidence for recent groundwater seepage and surface runoff on Mars". Science 288, 2330–2335.
- ^ Malin, M., K. Edgett, L. Posiolova, S. McColley, E. Dobrea. 2006. "Present-day impact cratering rate and contemporary gully activity on Mars". Science 314, 1573_1577.
- ^ Kolb, et al. 2010. "Investigating gully flow emplacement mechanisms using apex slopes". Icarus 2008, 132-142.
- ^ McEwen, A. et al. 2007. "A closer look at water-related geological activity on Mars". Science 317, 1706-1708.
- ^ Pelletier, J., et al. 2008. "Recent bright gully deposits on Mars wet or dry flow?" Geology 36, 211-214.
- ^ NASA/Jet Propulsion Laboratory. "NASA orbiter finds new gully channel on Mars". Science Daily, 22 March 2014.
- ^ "NASA Spacecraft Observes Further Evidence of Dry Ice Gullies on Mars". Jet Propulsion Laboratory.
- ^ "Activity in Martian Gullies". HiRISE: High Resolution Imaging Science Experiment. The University of Arizona: Lunar and Planetary Laboratory. 10 July 2014. Retrieved 7 January 2021.
- ^ "Gullies on Mars Carved by Dry Ice, Not Water". Space.com. 16 July 2014.
- ^ "Stones, Wind, and Ice: A Guide to Martian Impact Craters".
- ^ Hugh H. Kieffer (1992). Mars. University of Arizona Press. ISBN 978-0-8165-1257-7. Retrieved 7 March 2011.