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
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.
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]
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.
^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.
^"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".
arandas, crater, arandas, crater, mare, acidalium, quadrangle, mars, located, north, west, diameter, named, after, town, arandas, mexico, arandasarandas, crater, seen, hirise, click, image, better, view, north, south, walls, well, central, hills, scale, 1000, . 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 ArandasArandas 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 PlanetMarsCoordinates42 46 N 15 10 W 42 77 N 15 17 W 42 77 15 17 Coordinates 42 46 N 15 10 W 42 77 N 15 17 W 42 77 15 17QuadrangleMare AcidaliumDiameter24 76 km 15 39 mi EponymThe town of Arandas in MexicoViking orbiter mosaic of Arandas crater Detail of the ejecta of Arandas crater 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 Main article Martian Gullies 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 EditImpact event List of craters on Mars Mare Acidalium quadrangle Martian Gullies Ore resources on Mars Planetary nomenclature Water on MarsReferences 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 Portal Solar System Retrieved from https en wikipedia org w index php title Arandas crater amp oldid 1055138884, wikipedia, wiki, book, books, library,
