Difference between revisions of "Medusae Fossae"

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The '''Medusae Fossae Formation''' is a large geological formation of probable volcanic origin on the planet [[Mars]].<ref name=esa-mff>{{cite web|title=The Medusa Fossae formation on Mars|url=http://www.esa.int/Our_Activities/Space_Science/Mars_Express/The_Medusa_Fossae_formation_on_Mars/(print)|publisher=[[European Space Agency]]|date=29 March 2005}}</ref>
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The Medusae Fossae Formation is a large geological formation of probable volcanic origin on the planet [[Mars]].<ref> "The Medusa Fossae formation on Mars". European Space Agency. 29 March 2005.</ref>
  
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It is named for the [[Medusa (mythology)|Medusa]] of Greek mythology. "Fossae" is Latin for "trenches".  
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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&nbsp;km along the equator.
 
The formation is a collection of soft, easily eroded deposits that extends off and on for more than 5,000&nbsp;km along the equator.
  
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Its roughly-shaped regions extend from just south of [[Olympus Mons]] to [[Apollinaris Patera]], with a smaller additional region closer to [[Gale Crater]].<ref>{{Cite journal |author=Lujendra Ojha |author2=Kevin Lewis |author3=Suniti Karunatillake |author4=Mariek Schmidt|date=July 20, 2018|title=Fig. 1,
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Its roughly-shaped regions extend from just south of [[Olympus Mons]] to Apollinaris Patera, with a smaller additional region closer to [[Gale Crater]].<ref>Lujendra Ojha; Kevin Lewis; Suniti Karunatillake; Mariek Schmidt July 20, 2018 The Medusae Fossae Formation as the single largest source of dust on Mars". Nature Communications. ISSN 2041-1723.</ref>
  
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It has been determined that the Medusae Fossae Formation as the single largest source of dust on Mars|url=https://www.nature.com/articles/s41467-018-05291-5/figures/1|journal=Nature Communications|language=en|issn=2041-1723}}</ref>   
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It has been determined that the Medusae Fossae Formation as the single largest source of dust on Mars.<ref>
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|url=https://www.nature.com/articles/s41467-018-05291-5/figures/1|journal=Nature Communications|language=en|</ref>   
  
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The total area of the Medusae Fossae Formation is equal to 20% the size of the continental United States.<ref name="pmid30030425">{{cite journal |doi=10.1038/s41467-018-05291-5 |pmid=30030425 |pmc=6054634 |title=The Medusae Fossae Formation as the single largest source of dust on Mars |journal=Nature Communications |volume=9 |issue=1 |pages=2867 |year=2018 |last1=Ojha |first1=Lujendra |last2=Lewis |first2=Kevin |last3=Karunatillake |first3=Suniti |last4=Schmidt |first4=Mariek |bibcode=2018NatCo...9.2867O }}</ref>   
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The total area of the Medusae Fossae Formation is equal to 20% the size of the continental United States.<ref name="pmid30030425"> |pmid=30030425 |pmc=6054634 |title=The Medusae Fossae Formation as the single largest source of dust on Mars |journal=Nature Communications |volume=9 |issue=1 |pages=2867 |year=2018 |last1=Ojha |first1=Lujendra |last2=Lewis |first2=Kevin |last3=Karunatillake |first3=Suniti |last4=Schmidt |first4=Mariek |</ref>   
  
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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 quadrangle|Amazonis]], [[Tharsis quadrangle|Tharsis]], [[Memnonia quadrangle|Memnonia]], [[Elysium quadrangle|Elysium]], and [[Aeolis quadrangle|Aeolis]].
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The formation straddles what is called the  martian dichotomy|highland - lowland boundary near the Tharsis and Elysium volcanic areas, and extends across five quadrangles: [[Amazonis quadrangle|Amazonis]], [[Tharsis quadrangle|Tharsis]], [[Memnonia quadrangle|Memnonia]], [[Elysium quadrangle|Elysium]], and [[Aeolis quadrangle|Aeolis]].
  
 
== Origin and age ==
 
== Origin and age ==
 
The origin of the formation is unknown, but many theories have been presented over the years.
 
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]].<ref>Scientists Float a New Theory on the Medusae Fossae Formation". Eos. 19 May 2020.</ref>  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.<ref>{{cite journal |doi=10.1016/j.icarus.2012.03.016 |title=The dispersal of pyroclasts from ancient explosive volcanoes on Mars: Implications for the friable layered deposits |journal=Icarus |volume=219 |issue=1 |pages=358–381 |year=2012 |last1=Kerber |first1=Laura |last2=Head |first2=James W. |last3=Madeleine |first3=Jean-Baptiste |last4=Forget |first4=François |last5=Wilson |first5=Lionel | }}</ref> 
  
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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]].<ref>{{Cite web|title=Scientists Float a New Theory on the Medusae Fossae Formation|url=https://eos.org/articles/scientists-float-a-new-theory-on-the-medusae-fossae-formation|access-date=2021-06-26|website=Eos|date=19 May 2020 |language=en-US}}</ref>  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]].<ref>{{cite journal |doi=10.1016/j.icarus.2012.03.016 |title=The dispersal of pyroclasts from ancient explosive volcanoes on Mars: Implications for the friable layered deposits |journal=Icarus |volume=219 |issue=1 |pages=358–381 |year=2012 |last1=Kerber |first1=Laura |last2=Head |first2=James W. |last3=Madeleine |first3=Jean-Baptiste |last4=Forget |first4=François |last5=Wilson |first5=Lionel |bibcode=2012Icar..219..358K }}</ref>  
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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.<ref name="Ojha2018a">{{cite journal |doi=10.1029/2018JE005565 |title=The Density of the Medusae Fossae Formation: Implications for its Composition, Origin, and Importance in Martian History |journal=Journal of Geophysical Research: Planets |volume=123 |issue=6 |pages=1368–1379 |year=2018 |last1=Ojha |first1=Lujendra |last2=Lewis |first2=Kevin |</ref>
  
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The surface of the formation has been eroded by the wind into a series of linear ridges called yardangs.  The wind shapes things by bouncing sand particles.<ref>Bridges, Nathan T.; Muhs, Daniel R. (2012). "Duststones on Mars: Source, Transport, Deposition, and Erosion". Sedimentary Geology of Mars. pp. 169–182. doi:10.2110/pec.12.102.0169. ISBN 978-1-56576-312-8.</ref>  Layers are seen in parts of the formation. <ref>  |title=Sedimentary Geology of Mars |pages=169–182 |year=2012 |last1=Bridges |first1=Nathan T. |last2=Muhs |first2=Daniel R. |isbn=978-1-56576-312-8 }}</ref> 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.  Layers are seen in parts of the formation.
  
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Yardangs are common on Mars.<ref>Grotzinger, J. and R. Milliken (eds.)  2012.  Sedimentary Geology of Mars.  SEPM</ref>  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.<ref>name="hiroc.lpl.arizona.edu"</ref>
  
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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.<ref name="Ojha2018a">{{cite journal |doi=10.1029/2018JE005565 |title=The Density of the Medusae Fossae Formation: Implications for its Composition, Origin, and Importance in Martian History |journal=Journal of Geophysical Research: Planets |volume=123 |issue=6 |pages=1368–1379 |year=2018 |last1=Ojha |first1=Lujendra |last2=Lewis |first2=Kevin |bibcode=2018JGRE..123.1368O |doi-access=free }}</ref>
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[[Image:Aeolis Mensae Yardangs.JPG|left|thumb|400px|Aeolis Mensae Yardangs, as seen by HiRISE. Scale bar is 500 meters long. An inverted stream channel is also visible]]
  
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<gallery class="center"  widths="380px" heights="360px">
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File:Medusae map.jpg|Map of location of Medusae Fossae Formation
  
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The surface of the formation has been eroded by the wind into a series of linear ridges called [[yardang]]s.<ref>{{cite book |doi=10.2110/pec.12.102.0169 |chapter=Duststones on Mars: Source, Transport, Deposition, and Erosion |title=Sedimentary Geology of Mars |pages=169–182 |year=2012 |last1=Bridges |first1=Nathan T. |last2=Muhs |first2=Daniel R. |isbn=978-1-56576-312-8 }}</ref> 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]].
 
  
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Yardangs are parts of rock that have been sand blasted into long, skinny ridges by bouncing sand particles blowing in the wind.<ref>{{cite web | url=http://www.uahirise.org/ESP_039563_1730 | title=HiRISE &#124; Yardangs in Arsinoes Chaos (ESP_039563_1730) }}</ref> Layers are seen in parts of the formation.  A resistant caprock on the top of yardangs has been observed in Viking,<ref>{{cite journal |doi=10.1029/JB087iB02p01179 |title=Ignimbrites of Amazonis Planitia Region of Mars |journal=Journal of Geophysical Research: Solid Earth |volume=87 |pages=1179–1190 |year=1982 |last1=Scott |first1=David H. |last2=Tanaka |first2=Kenneth L. |bibcode=1982JGR....87.1179S }}</ref> [[Mars Global Surveyor]],<ref>{{cite journal |doi=10.1126/science.279.5357.1681 |title=Early Views of the Martian Surface from the Mars Orbiter Camera of Mars Global Surveyor |journal=Science |volume=279 |issue=5357 |pages=1681–1685 |year=1998 |last1=Malin |first1=M. C. |last2=Carr |first2=M. H. |last3=Danielson |first3=G. E. |last4=Davies |first4=M. E. |last5=Hartmann |first5=W. K. |last6=Ingersoll |first6=A. P. |last7=James |first7=P. B. |last8=Masursky |first8=H. |last9=McEwen |first9=A. S. |last10=Soderblom |first10=L. A. |last11=Thomas |first11=P. |last12=Veverka |first12=J. |last13=Caplinger |first13=M. A. |last14=Ravine |first14=M. A. |last15=Soulanille |first15=T. A. |last16=Warr En |first16=J. L. |bibcode=1998Sci...279.1681M |pmid=9497280 |doi-access= }}</ref> and [[HiRISE]] photos.<ref>{{cite journal |doi=10.1029/2008JE003076 |title=Origin of the Medusae Fossae Formation, Mars: Insights from a synoptic approach |journal=Journal of Geophysical Research |volume=113 |issue=E12 |pages=E12011 |year=2008 |last1=Mandt |first1=Kathleen E. |last2=De Silva |first2=Shanaka L. |last3=Zimbelman |first3=James R. |last4=Crown |first4=David A. |bibcode=2008JGRE..11312011M |doi-access=free }}</ref>
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</gallery>
  
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==Yardangs==
 
  
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Yardangs are common on Mars.<ref>Grotzinger, J. and R. Milliken (eds.)  2012. Sedimentary Geology of Mars. SEPM</ref>  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.<ref>name="hiroc.lpl.arizona.edu"</ref>  Yardangs are common in the Medusae Fossae Formation on Mars.
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<gallery class="center"  widths="380px" heights="360px">
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File:61167 1735yardangs3.jpg|Yardangs
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[[Image:Aeolis Mensae Yardangs.JPG|left|thumb|400px|Aeolis Mensae Yardangs, as seen by HiRISE.  Scale bar is 500 meters long. An inverted stream channel is also visible]]
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File:35558 1830yardangs.jpg|Yardangs in Amazonis quadrangle
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File:ESP 045831 1750yardangswide.jpg|Wide view of yardangs in Amazonis quadrangle
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File:ESP 045831 1750yardangscolor.jpg|Close, color view of yardangs in Amazonis quadrangle
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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.<ref>{{cite web | url=http://themis.asu.edu/zoom-20020416a | title=Medusae Fossae Formation &#124; Mars Odyssey Mission THEMIS }}</ref>
  
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<gallery class="center"  widths="380px" heights="360px">
 
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File:Medusae map.jpg|Map of location of Medusae Fossae Formation
 
 
Image:Apollinarisandmedusae.JPG|Medusae Fossae Formation southeast of Apollinaris Patera
 
Image:Apollinarisandmedusae.JPG|Medusae Fossae Formation southeast of Apollinaris Patera
  
 
File: ESP 051978 1720yardangslayers.jpg|Small yardangs
 
File: ESP 051978 1720yardangslayers.jpg|Small yardangs
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</gallery>
 
</gallery>
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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 (geology)|cementation]]. Very few [[impact craters]] are visible throughout the area so the surface is relatively young.<ref>{{cite web | url=http://themis.asu.edu/zoom-20020416a | title=Medusae Fossae Formation &#124; Mars Odyssey Mission THEMIS }}</ref>
 
  
 
==See also==
 
==See also==
Line 59: Line 60:
  
 
* [https://www.youtube.com/watch?v=_sUUKcZaTgA Martian Ice - Jim Secosky - 16th Annual International Mars Society Convention]
 
* [https://www.youtube.com/watch?v=_sUUKcZaTgA Martian Ice - Jim Secosky - 16th Annual International Mars Society Convention]
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* 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
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*
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* 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]
 
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* [https://www.youtube.com/watch?v=m2ERsEXAq_s  - Jeffrey Plaut - Subsurface Ice - 21st Annual International Mars Society Convention-2018]
 
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==References==
 
==References==
 
{{reflist|colwidth=30em}}
 
{{reflist|colwidth=30em}}

Latest revision as of 07:29, 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]

It has been determined that the Medusae Fossae Formation as the single largest source of dust on Mars.[3]

The total area of the Medusae Fossae Formation is equal to 20% the size of the continental United States.[4]

The formation straddles what is called the martian dichotomy|highland - lowland boundary near the Tharsis and 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.[5] 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.[6]

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.[7]

The surface of the formation has been eroded by the wind into a series of linear ridges called yardangs. The wind shapes things by bouncing sand particles.[8] Layers are seen in parts of the formation. [9] 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. Layers are seen in parts of the formation.

Yardangs are common on Mars.[10] 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.[11]

Aeolis Mensae Yardangs, as seen by HiRISE. Scale bar is 500 meters long. An inverted stream channel is also visible

  • Map of location of Medusae Fossae Formation


  • Yardangs

  • Yardangs in Amazonis quadrangle

  • Wide view of yardangs in Amazonis quadrangle

  • Close, color view of yardangs in Amazonis quadrangle

  • Medusae Fossae Formation southeast of Apollinaris Patera

  • Small yardangs

See also

External links

References

  1. ↑ "The Medusa Fossae formation on Mars". European Space Agency. 29 March 2005.
  2. ↑ Lujendra Ojha; Kevin Lewis; Suniti Karunatillake; Mariek Schmidt July 20, 2018 The Medusae Fossae Formation as the single largest source of dust on Mars". Nature Communications. ISSN 2041-1723.
  3. ↑ |url=https://www.nature.com/articles/s41467-018-05291-5/figures/1%7Cjournal=Nature Communications|language=en|
  4. ↑ |pmid=30030425 |pmc=6054634 |title=The Medusae Fossae Formation as the single largest source of dust on Mars |journal=Nature Communications |volume=9 |issue=1 |pages=2867 |year=2018 |last1=Ojha |first1=Lujendra |last2=Lewis |first2=Kevin |last3=Karunatillake |first3=Suniti |last4=Schmidt |first4=Mariek |
  5. ↑ Scientists Float a New Theory on the Medusae Fossae Formation". Eos. 19 May 2020.
  6. ↑ "The dispersal of pyroclasts from ancient explosive volcanoes on Mars: Implications for the friable layered deposits" (2012). Icarus 219 (1): 358–381. doi:10.1016/j.icarus.2012.03.016. 
  7. ↑ "Sedimentary Geology of Mars" (2012). Journal of Geophysical Research: Planets 123 (6): 169–182. doi:10.1029/2018JE005565. 
  8. ↑ Grotzinger, J. and R. Milliken (eds.) 2012. Sedimentary Geology of Mars. SEPM
  9. ↑ name="hiroc.lpl.arizona.edu"
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