Difference between revisions of "Medusae Fossae"
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Revision as of 05:21, 8 January 2024
The Medusae Fossae Formation is a large geological formation of probable volcanic origin on the planet Mars.[1]
It is named for the Medusa of Greek mythology. "Fossae" is Latin for "trenches".
The formation is a collection of soft, easily eroded deposits that extends off and on for more than 5,000 km along the equator.
Its roughly-shaped regions extend from just south of Olympus Mons to Apollinaris Patera, with a smaller additional region closer to Gale Crater.[2]
The total area of the Medusae Fossae Formation is equal to 20% the size of the continental United States.[3]
The formation straddles what is called the martian dichotomy|highland - lowland boundary near the Tharsis and Elysium (volcanic province)|Elysium volcanic areas, and extends across five quadrangles: Amazonis, Tharsis, Memnonia, Elysium, and Aeolis.
Origin and age
The origin of the formation is unknown, but many theories have been presented over the years.
In 2020, a group of researchers headed by Peter Mouginis-Mark has hypothesized that the formation could have been formed from pumice rafts from the volcano Olympus Mons.[4] In 2012, a group headed by Laura Kerber hypothesized that it could have been formed from ash from the volcanoes Apollinaris Mons, Arsia Mons, and possibly Pavonis Mons.[5]
Its density and high content of sulfur and chlorine, suggests an explosive volcanic origin. It may have been deposited in periodic eruptions over an interval of 500 million years.[6]
The surface of the formation has been eroded by the wind into a series of linear ridges called yardangs.[7] These ridges generally point in direction of the prevailing winds that carved them, and demonstrate the erosive power of Martian winds. The easily eroded nature of the Medusae Fossae Formation suggests that it is composed of weakly cemented particles, and was most likely formed by the deposition of wind-blown dust or volcanic ash.
Yardangs are parts of rock that have been sand blasted into long, skinny ridges by bouncing sand particles blowing in the wind.[8] Layers are seen in parts of the formation. A resistant caprock on the top of yardangs has been observed in Viking,[9] Mars Global Surveyor,[10] and HiRISE photos.[11]
Yardangs
Yardangs are common on Mars.[12] They are generally visible as a series of parallel linear ridges. Their parallel nature is thought to be caused by the direction of the prevailing wind.[13] Yardangs are common in the Medusae Fossae Formation on Mars.
- Medusae Fossae Formation
Map of location of Medusae Fossae Formation
Medusae Fossae Formation southeast of Apollinaris Patera
Small yardangs
Images from spacecraft show that they have different degrees of hardness probably because of significant variations in the physical properties, composition, particle size, and/or cementation. Very few impact craters are visible throughout the area so the surface is relatively young.[14]
See also
- Dark slope streaks
- Geography of Mars
- High Resolution Imaging Science Experiment (HiRISE)
- HiWish program
- How are features on Mars Named?
- Glaciers on Mars
- Layers on Mars
- Mars Global Surveyor
- Martian features that are signs of water ice
- Martian gullies
- Oceans on Mars
- Periodic climate changes on Mars
- Rivers on Mars
- Sublimation landscapes on Mars
External links
- Martian Ice - Jim Secosky - 16th Annual International Mars Society Convention
- https://www.youtube.com/watch?v=kpnTh3qlObk T. Gordon Wasilewski - Water on Mars - 20th Annual International Mars Society Convention] Describes how to get water from ice in the ground
- https://www.youtube.com/watch?v=PYl3HXpvqhM Kris Zacny Water on Mars - 21st Annual International Mars Society Convention Describes how to get water from ice in the ground]
References
- ↑ Template:Cite web
- ↑ Lujendra Ojha (July 20, 2018). "[https://www.nature.com/articles/s41467-018-05291-5/figures/1 Fig. 1, It has been determined that the Medusae Fossae Formation as the single largest source of dust on Mars]" (in en). Nature Communications. ISSN 2041-1723.
- ↑ "The Medusae Fossae Formation as the single largest source of dust on Mars" (2018). Nature Communications 9 (1): 2867. doi:. PMID 30030425. Bibcode: 2018NatCo...9.2867O.
- ↑ Template:Cite web
- ↑ "The dispersal of pyroclasts from ancient explosive volcanoes on Mars: Implications for the friable layered deposits" (2012). Icarus 219 (1): 358–381. doi:. Bibcode: 2012Icar..219..358K.
- ↑ "The Density of the Medusae Fossae Formation: Implications for its Composition, Origin, and Importance in Martian History" (2018). Journal of Geophysical Research: Planets 123 (6): 1368–1379. doi:. Bibcode: 2018JGRE..123.1368O.
- ↑ Template:Cite book
- ↑ Template:Cite web
- ↑ "Ignimbrites of Amazonis Planitia Region of Mars" (1982). Journal of Geophysical Research: Solid Earth 87: 1179–1190. doi:. Bibcode: 1982JGR....87.1179S.
- ↑ "Early Views of the Martian Surface from the Mars Orbiter Camera of Mars Global Surveyor" (1998). Science 279 (5357): 1681–1685. doi:. PMID 9497280. Bibcode: 1998Sci...279.1681M.
- ↑ "Origin of the Medusae Fossae Formation, Mars: Insights from a synoptic approach" (2008). Journal of Geophysical Research 113 (E12): E12011. doi:. Bibcode: 2008JGRE..11312011M.
- ↑ Grotzinger, J. and R. Milliken (eds.) 2012. Sedimentary Geology of Mars. SEPM
- ↑ name="hiroc.lpl.arizona.edu"
- ↑ Template:Cite web
