Difference between revisions of "Hellas Planitia"

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Also, the shapes of many features in Hellas Planitia and other parts of Mars are strongly suggestive of glaciers, as the surface looks as if movement has taken place.
 
Also, the shapes of many features in Hellas Planitia and other parts of Mars are strongly suggestive of glaciers, as the surface looks as if movement has taken place.
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==Honeycomb Terrain==
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Honeycomb terrain bears shapes similar to a honeycomb.  This “honeycomb” terrain was first discovered in the northwestern part of the floor of Hellas.<ref name="ReferenceB">{{cite journal | last1 = Bernhardt | first1 = H. | display-authors = etal  | year = 2016 | title = The honeycomb terrain on the Hellas basin floor, mars: a case for salt or ice diapirism: hellas honeycombs as salt/ice diapirs | url = | journal = J. Geophys. Res. | volume = 121 | issue = | pages = 714–738 | doi=10.1002/2016je005007| bibcode = 2016JGRE..121..714B}}</ref>  The geologic process responsible for creating these features remains unresolved.<ref>http://www.uahirise.org/ESP_049330_1425</ref>  Some calculations indicate that this formation may have been caused by ice moving up through the ground in this region.  The ice layer would have been between 100 m and 1&nbsp;km thick.<ref>Weiss, D., J. Head.  2017.  HYDROLOGY OF THE HELLAS BASIN AND THE EARLY MARS CLIMATE: WAS THE HONEYCOMB TERRAIN FORMED BY SALT OR ICE DIAPIRISM?  Lunar and Planetary Science XLVIII. 1060.pdf</ref><ref>{{cite journal | last1 = Weiss | first1 = D. | last2 = Head | first2 = J. | year = 2017 | title = Salt or ice diapirism origin for the honeycomb terrain in Hellas basin, Mars?: Implications for the early martian climate | url = | journal = Icarus | volume = 284 | issue = | pages = 249–263 | doi=10.1016/j.icarus.2016.11.016 | bibcode=2017Icar..284..249W}}</ref><ref name="ReferenceB"/>  So, it seems that large masses of ice have pushed up layers of rock into domes that were eroded.  After erosion removed the top of the layered domes, circular features remained that look like the cells in a honeycomb.
  
  

Revision as of 10:40, 8 February 2018

A Mars Orbiter Laser Altimeter (MOLA) image (onboard the Mars Global Surveyor orbiter) of Hellas Planitia.
Map showing locations of Hellas Planitia and other nearby regions

Hellas Planitia is a vast meteorite impact basin located at 42° 42'S 70° 00'E, in the Mars southern hemisphere. Hellas Planitia is in the Hellas quadrangle and the Noachis quadrangle. Also known as the Hellas Impact Basin, this landmark has a very obvious impact crater ring 2,300 km (1,400 mi) in diameter. This is one of the largest known impact craters in the solar system.[1][2]

Radar images by the Mars Reconnaissance Orbiter (MRO) spacecraft's SHARAD radar sounder suggest that features called lobate debris aprons in at least some craters in the eastern region of Hellas Planitia are actually glaciers of water ice lying buried beneath thin layers of dirt and rock.[3] Scientists believe that snow and ice accumulated on higher topography, flowed downhill, and is now protected from sublimation by a layer of rock debris and dust. Sublimation is when a solid changes directly to a gas without passing through a liquid phase. So on Mars, water ice will go directly into a vapor phase. This is common on Mars because of its thin atmosphere. Furrows and ridges on the surface were caused by deforming ice.

Also, the shapes of many features in Hellas Planitia and other parts of Mars are strongly suggestive of glaciers, as the surface looks as if movement has taken place.

Honeycomb Terrain

Honeycomb terrain bears shapes similar to a honeycomb. This “honeycomb” terrain was first discovered in the northwestern part of the floor of Hellas.[4] The geologic process responsible for creating these features remains unresolved.[5] Some calculations indicate that this formation may have been caused by ice moving up through the ground in this region. The ice layer would have been between 100 m and 1 km thick.[6][7][4] So, it seems that large masses of ice have pushed up layers of rock into domes that were eroded. After erosion removed the top of the layered domes, circular features remained that look like the cells in a honeycomb.


Channels in Hellas quadrangle
Honeycomb terrain on floor of Hellas Basin
Tongue-shaped glacier in Hellas Planitia


References:

  1. Hellas Basin article on Wikipedia
  2. Impact Craters on Wikipedia
  3. Template:Cite web
  4. 4.0 4.1 "The honeycomb terrain on the Hellas basin floor, mars: a case for salt or ice diapirism: hellas honeycombs as salt/ice diapirs" (2016). J. Geophys. Res. 121: 714–738. doi:10.1002/2016je005007. Bibcode2016JGRE..121..714B. 
  5. http://www.uahirise.org/ESP_049330_1425
  6. Weiss, D., J. Head. 2017. HYDROLOGY OF THE HELLAS BASIN AND THE EARLY MARS CLIMATE: WAS THE HONEYCOMB TERRAIN FORMED BY SALT OR ICE DIAPIRISM? Lunar and Planetary Science XLVIII. 1060.pdf
  7. "Salt or ice diapirism origin for the honeycomb terrain in Hellas basin, Mars?: Implications for the early martian climate" (2017). Icarus 284: 249–263. doi:10.1016/j.icarus.2016.11.016. Bibcode2017Icar..284..249W. 



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