Difference between revisions of "Margaritifer Terra"
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| − | Margaritifer Terra is a heavily cratered region of Mars. It is centered just south of the Martian equator at 4.9 S and 25 W (335 E) and covers 2600 km at its widest extent.<ref>^ Margaritifer Terra. Gazetteer of Planetary Nomenclature. USGS Astrogeology Research Program.</ref> The area displays chaos terrain, outflow channels, and alluvial plains that are evidence of massive flooding. A region within the terra shows some of the highest valley network densities on the planet. Ares Vallis is one place where the flood and flow patterns are in evidence; it was the landing site of NASA's ''Mars Pathfinder. It is also one of several proposed landing sites for the Mars 2020 Rover.<ref>https://asunews.asu.edu/20140516-mars-2020 |title=Choosing a place to land NASA's next Mars rover |work=Arizona State University News</ref> | + | [[Image: Wikimolaargyre.jpg|thumb|600px|left|MOLA map showing boundaries for Margaritifer Terra and other regions. Color indicates elevation. |
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| + | Margaritifer Terra is a heavily cratered region of Mars. It is centered just south of the Martian equator at 4.9 S and 25 W (335 E) and covers 2600 km at its widest extent.<ref>^ Margaritifer Terra. Gazetteer of Planetary Nomenclature. USGS Astrogeology Research Program.</ref> The area displays chaos terrain, outflow channels, and alluvial plains that are evidence of massive flooding. A region within the terra shows some of the highest valley network densities on the planet. Ares Vallis is one place where the flood and flow patterns are in evidence; it was the landing site of NASA's ''Mars Pathfinder." It is also one of several proposed landing sites for the Mars 2020 Rover.<ref>https://asunews.asu.edu/20140516-mars-2020 |title=Choosing a place to land NASA's next Mars rover |work=Arizona State University News</ref> | ||
Margaritifer Terra was named in 1979, after the Pearl Fishery Coast, south India. Part of it is found in the Margaritifer Sinus quadrangle and part in the Oxia Palus quadrangle. | Margaritifer Terra was named in 1979, after the Pearl Fishery Coast, south India. Part of it is found in the Margaritifer Sinus quadrangle and part in the Oxia Palus quadrangle. | ||
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One of the first images released under NASA's HiWish program was of layered mesas in Aureum Chaos.<ref>http://www.uahirise.org/releases/hiwish-captions.php Captioned Images Inspired by HiWish Suggestions (HiRISE)</ref> | One of the first images released under NASA's HiWish program was of layered mesas in Aureum Chaos.<ref>http://www.uahirise.org/releases/hiwish-captions.php Captioned Images Inspired by HiWish Suggestions (HiRISE)</ref> | ||
| − | <gallery class="center" widths="230px" heights="220px" > | + | <gallery class="center" widths="230px" heights="220px"> |
Image: Aureum Chaos wide view.jpg|Aureum Chaos, as seen by HiRISE, under the HiWish program. This was one of the first images from the HiWish program. | Image: Aureum Chaos wide view.jpg|Aureum Chaos, as seen by HiRISE, under the HiWish program. This was one of the first images from the HiWish program. | ||
</gallery> | </gallery> | ||
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A detailed discussion of layering with many Martian examples can be found in Sedimentary Geology of Mars.<ref>Grotzinger, J. and R. Milliken (eds.). 2012. Sedimentary Geology of Mars. SEPM.</ref> | A detailed discussion of layering with many Martian examples can be found in Sedimentary Geology of Mars.<ref>Grotzinger, J. and R. Milliken (eds.). 2012. Sedimentary Geology of Mars. SEPM.</ref> | ||
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| + | [[File: 24807whitebuttei.jpg|thumb|500px|left|Enlargement of white butte, as seen by HiRISE under HiWish program. Box shows size of a football field.]] | ||
| − | Holden Crater and Eberswalde Crater | + | Holden Crater and Eberswalde Crater (craters in this region) are thought to have once held lakes because they contain deltas and minerals which need water to form.<ref>Murchie, S. et al. 2009. A synthesis of Martian aqueous mineralogy after 1 Mars year of observations from the Mars Reconnaissance Orbiter. Journal of Geophysical Research: 114.</ref> The Uzboi-Landon-Morava (ULM) system of paths for water flow is found in Margaritifer Terra. |
==References== | ==References== | ||
{{Reflist}} | {{Reflist}} | ||
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| + | ==See also== | ||
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| + | *[[High Resolution Imaging Science Experiment (HiRISE)]] | ||
| + | *[[HiWish program]] | ||
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| + | *[[Layers on Mars]] | ||
| + | *[[Margaritifer Sinus quadrangle]] | ||
| + | *[[Mars Global Surveyor]] | ||
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| + | *[[Rivers on Mars]] | ||
==External links== | ==External links== | ||
* [https://www.youtube.com/watch?v=DGBbke1wJRk] Lakes on Mars - Nathalie Cabrol (SETI Talks) | * [https://www.youtube.com/watch?v=DGBbke1wJRk] Lakes on Mars - Nathalie Cabrol (SETI Talks) | ||
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| + | [[Category:Mars Atlas]] | ||
Latest revision as of 05:47, 23 March 2020
Margaritifer Terra is a heavily cratered region of Mars. It is centered just south of the Martian equator at 4.9 S and 25 W (335 E) and covers 2600 km at its widest extent.[1] The area displays chaos terrain, outflow channels, and alluvial plains that are evidence of massive flooding. A region within the terra shows some of the highest valley network densities on the planet. Ares Vallis is one place where the flood and flow patterns are in evidence; it was the landing site of NASA's Mars Pathfinder." It is also one of several proposed landing sites for the Mars 2020 Rover.[2]
Margaritifer Terra was named in 1979, after the Pearl Fishery Coast, south India. Part of it is found in the Margaritifer Sinus quadrangle and part in the Oxia Palus quadrangle.
One of the first images released under NASA's HiWish program was of layered mesas in Aureum Chaos.[3]
Aureum Chaos, as seen by HiRISE, under the HiWish program. This was one of the first images from the HiWish program.
Some of the images from this region display layers. Many places on Mars show rocks arranged in layers. Rock can form layers in a variety of ways. Volcanoes, wind, or water can produce layers.[4] A detailed discussion of layering with many Martian examples can be found in Sedimentary Geology of Mars.[5]
Holden Crater and Eberswalde Crater (craters in this region) are thought to have once held lakes because they contain deltas and minerals which need water to form.[6] The Uzboi-Landon-Morava (ULM) system of paths for water flow is found in Margaritifer Terra.
References
- ↑ ^ Margaritifer Terra. Gazetteer of Planetary Nomenclature. USGS Astrogeology Research Program.
- ↑ https://asunews.asu.edu/20140516-mars-2020 |title=Choosing a place to land NASA's next Mars rover |work=Arizona State University News
- ↑ http://www.uahirise.org/releases/hiwish-captions.php Captioned Images Inspired by HiWish Suggestions (HiRISE)
- ↑ http://hirise.lpl.arizona.edu?PSP_008437_1750 |title=HiRISE | High Resolution Imaging Science Experiment |publisher=Hirise.lpl.arizona.edu?psp_008437_1750
- ↑ Grotzinger, J. and R. Milliken (eds.). 2012. Sedimentary Geology of Mars. SEPM.
- ↑ Murchie, S. et al. 2009. A synthesis of Martian aqueous mineralogy after 1 Mars year of observations from the Mars Reconnaissance Orbiter. Journal of Geophysical Research: 114.
See also
External links
- [1] Lakes on Mars - Nathalie Cabrol (SETI Talks)
