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'''Martian "spiders"''' (also called ]s, dark spots and Dalmatian spots)<ref> {{Citation| first= | last=| coauthors=| contribution=POSSIBLE LIQUID-LIKE WATER PRODUCED SEEPAGE FEATURES ON MARS.| title=40th. Lunar and Planetary Science Conference (2009)| editor-first=A.| editor-last=Kereszturi| coeditors=''et al.''| publisher=| place=| pages=| date=| year=2009| id= | contribution-url=http://www.lpi.usra.edu/meetings/lpsc2009/pdf/1111.pdf| format=PDF| accessdate=2009-08-12 }}</ref><ref name=2006-100 > {{cite news | first= | last= | coauthors= |authorlink= | title=NASA Findings Suggest Jets Bursting From Martian Ice Cap | date=August 16, 2006 | publisher=NASA | url =http://www.jpl.nasa.gov/news/news.cfm?release=2006-100 | work =Jet Propulsion Laboratory | pages = | accessdate = 2009-08-11 | language = }}</ref><ref> {{Citation| first= | last=| coauthors=| contribution=STRATIGRAPHY OF SPECIAL LAYERS – TRANSIENT ONES ON PERMEABLE ONES: EXAMPLES| title=Lunar and Planetary Science XXXV (2004)| editor-first=Sz.| editor-last=Bérczi| coeditors=''et al.''| publisher=| place=| pages=| date=| year=2004| id= | contribution-url=http://www.lpi.usra.edu/meetings/lpsc2004/pdf/1317.pdf| format=PDF| accessdate=2009-08-12 }}</ref> are geological formations thus far unique to the ] of ]. These structures have not been found in the ] or any other region of Mars to date. They appear as the ] ice cap at the Martian south pole ] into carbon dioxide gas during the Martian spring and the surface below is revealed. '''Martian "spiders"''' (also called ]s, dark spots and Dalmatian spots)<ref> {{Citation| first= | last=| coauthors=| contribution=POSSIBLE LIQUID-LIKE WATER PRODUCED SEEPAGE FEATURES ON MARS.| title=40th. Lunar and Planetary Science Conference (2009)| editor-first=A.| editor-last=Kereszturi| coeditors=''et al.''| publisher=| place=| pages=| date=| year=2009| id= | contribution-url=http://www.lpi.usra.edu/meetings/lpsc2009/pdf/1111.pdf| format=PDF| accessdate=2009-08-12 }}</ref><ref name=2006-100 > {{cite news | first= | last= | coauthors= |authorlink= | title=NASA Findings Suggest Jets Bursting From Martian Ice Cap | date=August 16, 2006 | publisher=NASA | url =http://www.jpl.nasa.gov/news/news.cfm?release=2006-100 | work =Jet Propulsion Laboratory | pages = | accessdate = 2009-08-11 | language = }}</ref><ref name=clathrate > {{Citation| first= | last=| coauthors=| contribution=STRATIGRAPHY OF SPECIAL LAYERS – TRANSIENT ONES ON PERMEABLE ONES: EXAMPLES| title=Lunar and Planetary Science XXXV (2004)| editor-first=Sz.| editor-last=Bérczi| coeditors=''et al.''| publisher=| place=| pages=| date=| year=2004| id= | contribution-url=http://www.lpi.usra.edu/meetings/lpsc2004/pdf/1317.pdf| format=PDF| accessdate=2009-08-12 }}</ref> are geological formations thus far unique to the ] of ]. These structures have not been found in the ] or any other region of Mars to date. They appear as the ] ice cap at the Martian south pole ] into carbon dioxide gas during the Martian spring and the surface below is revealed.


The formations, when viewed individually, form a round lobed structure reminiscent of a spider web. They generally radiate outward in lobes from a central point.<ref name=AIG > {{cite web|url=http://www.aig.asn.au/pdf/AIGnews_Aug06.pdf |title=Spiders on Earth and Mars (pp. 21)|accessdate=2009-08-11 |date=August 2006 |format=PDF |publisher=Australian Institute of Geoscientists }}</ref> The central point is sometimes, but not always, a crater.<ref> Photographic examples: , , </ref> The formation is similar in its branching appearance to ]. The formations, when viewed individually, form a round lobed structure reminiscent of a spider web. They generally radiate outward in lobes from a central point.<ref name=AIG > {{cite web|url=http://www.aig.asn.au/pdf/AIGnews_Aug06.pdf |title=Spiders on Earth and Mars (pp. 21)|accessdate=2009-08-11 |date=August 2006 |format=PDF |publisher=Australian Institute of Geoscientists }}</ref> The central point is sometimes, but not always, a crater.<ref> Photographic examples: , , </ref> The formation is similar in its branching appearance to ].
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]. This one may be about 500 m in diameter and 1 m deep.]] ]. This one may be about 500 m in diameter and 1 m deep.]]
Some theories include: Some theories include:
*Dry venting of carbon dioxide (CO<sub>2</sub>) gas and sand. As the southern spring CO<sub>2</sub> ice receives enough Sun energy, it starts subliming the CO<sub>2</sub> ice from the bottom. This vapor accumulates under the slab rapidly increasing pressure and erupting.<ref name=2006-100 /><ref name=Portyankina /> High-pressure gas roars through at speeds of 161&nbsp;km/h (100 m/h) or more; under the slab, the gas erodes ground as it rushes toward the vents, snatching up loose particles of sand and carving the spidery network of grooves. The dark material falls back to the surface, creating dark patches and patterns on the ice cap. *Dry venting of carbon dioxide (CO<sub>2</sub>) gas and sand. As the southern spring CO<sub>2</sub> ice receives enough Sun energy, it starts subliming the CO<sub>2</sub> ice from the bottom. This vapor accumulates under the slab rapidly increasing pressure and erupting.<ref name=2006-100 /><ref name=Portyankina /> High-pressure gas roars through at speeds of 161&nbsp;km/h (100 m/h) or more; under the slab, the gas erodes ground as it rushes toward the vents, snatching up loose particles of sand and carving the spidery network of grooves. The dark material falls back to the surface, creating dark patches and patterns on the ice cap.
*Atmospheric pressure. On Mars the surface atmospheric pressure varies annually around: 6.7-8.8 mbar and 7.5-9.7 mbar; daily around 6.4-6.8 mbar. Because of the pressure changes subsurface gases expand and contract periodically, causing a downward gas flow during increase of and upward flow during decrease of atmospheric pressure.<ref name=clathrate />
*Active water-driven erosive structures. Water derived from sub-surface layers is expelled up fissures eroding joints to create tributaries capped with mud-like material and/or ice.<ref>Spiders: . Prieto-Ballesteros, Olga ''et al.'' '''Astrobiology'''. August 2006, Vol. 6, No. 4. pp: 651-667</ref><ref> {{cite journal|title=Martian Spiders as feasible water-driven erosive structures|journal=Centro de Astrobiología-INTA-CSIC|date=2005|first=Olga|last=Prieto-Ballesteros|coauthors=|volume=|issue=|pages=|id= |url=http://nai.nasa.gov/nai2005/abstracts/653%20-%20NAI2005-spiders.doc.pdf|format=|accessdate=2009-08-11 }}</ref> *Active water-driven erosive structures. Water derived from sub-surface layers is expelled up fissures eroding joints to create tributaries capped with mud-like material and/or ice.<ref>Spiders: . Prieto-Ballesteros, Olga ''et al.'' '''Astrobiology'''. August 2006, Vol. 6, No. 4. pp: 651-667</ref><ref> {{cite journal|title=Martian Spiders as feasible water-driven erosive structures|journal=Centro de Astrobiología-INTA-CSIC|date=2005|first=Olga|last=Prieto-Ballesteros|coauthors=|volume=|issue=|pages=|id= |url=http://nai.nasa.gov/nai2005/abstracts/653%20-%20NAI2005-spiders.doc.pdf|format=|accessdate=2009-08-11 }}</ref>
*Modified ] model: Structures form as the outside of the flow chills.{{Citation needed|August 2008|date=August 2009}} *] model: Structures form as the outside of the flow chills.<ref name=clathrate />


It has also previously been suggested that these structures had a volcanic cause {{Citation needed|date=February 2007}} or were simply warm patches of bare ground, however recent thermal imaging by NASA has revealed that these structures are generally as cold as the dry ice that covers the area during the Martian southern hemispheric winter.<ref name=2006-100 /> It has also previously been suggested that these structures had a volcanic cause {{Citation needed|date=February 2007}} or were simply warm patches of bare ground, however recent thermal imaging by NASA has revealed that these structures are generally as cold as the dry ice that covers the area during the Martian southern hemispheric winter.<ref name=2006-100 />

Revision as of 02:46, 12 August 2009

It has been suggested that this article be merged with Dark dune spot and Talk:Martian spiders#Merger proposal. (Discuss) Proposed since August 2009.
Original caption released with image: A delicate pattern, like that of a spider web, appears on top of the Mars residual polar cap, after the seasonal carbon-dioxide ice slab has disappeared. Next spring, these will likely mark the sites of vents when the carbon-dioxide ice cap returns. This Mars Global Surveyor, Mars Orbiter Camera image is about 3-kilometers wide (2-miles). Image courtesy of NASA/JPL-Caltech.

Martian "spiders" (also called dark dune spots, dark spots and Dalmatian spots) are geological formations thus far unique to the south polar region of Mars. These structures have not been found in the north polar region or any other region of Mars to date. They appear as the carbon dioxide ice cap at the Martian south pole sublimates into carbon dioxide gas during the Martian spring and the surface below is revealed.

The formations, when viewed individually, form a round lobed structure reminiscent of a spider web. They generally radiate outward in lobes from a central point. The central point is sometimes, but not always, a crater. The formation is similar in its branching appearance to diffusion-limited aggregation.

Causes

Soon after the first detection in 2005, they were discovered to be negative topographical features - i.e. radial troughs or channels. This unusual shape and appearance of "spiders" caused a lot of speculation about their origin. The reasons for their geographic distribution is still unknown. Their boundary does not correlate with any other properties of the surface such as elevation, geological structure, chemical composition or thermal properties.

Some investigators have suggested that the "spiders" are dendritic drainage channels. But one characteristic that makes the formations so difficult to explain is the way they "work against" gravity. In fact, the branching occurs radially from a center, positively excluding a drainage function. Moreover, the spiders form in identical shapes irrespective of the terrain. Often, a single ravine is seen moving both uphill and down, and many of these radial patterns occur on a consistent incline.

A 'spider', also called 'Star burst Channels', as seen by HiRISE. This one may be about 500 m in diameter and 1 m deep.

Some theories include:

  • Dry venting of carbon dioxide (CO2) gas and sand. As the southern spring CO2 ice receives enough Sun energy, it starts subliming the CO2 ice from the bottom. This vapor accumulates under the slab rapidly increasing pressure and erupting. High-pressure gas roars through at speeds of 161 km/h (100 m/h) or more; under the slab, the gas erodes ground as it rushes toward the vents, snatching up loose particles of sand and carving the spidery network of grooves. The dark material falls back to the surface, creating dark patches and patterns on the ice cap.
  • Atmospheric pressure. On Mars the surface atmospheric pressure varies annually around: 6.7-8.8 mbar and 7.5-9.7 mbar; daily around 6.4-6.8 mbar. Because of the pressure changes subsurface gases expand and contract periodically, causing a downward gas flow during increase of and upward flow during decrease of atmospheric pressure.
  • Active water-driven erosive structures. Water derived from sub-surface layers is expelled up fissures eroding joints to create tributaries capped with mud-like material and/or ice.
  • Clathrate hydrate model: Structures form as the outside of the flow chills.

It has also previously been suggested that these structures had a volcanic cause or were simply warm patches of bare ground, however recent thermal imaging by NASA has revealed that these structures are generally as cold as the dry ice that covers the area during the Martian southern hemispheric winter. NASA press release from August 16, 2006 states that an earlier theory proposed that the spots were patches of warm, bare ground exposed as the ice disappeared. However, the camera on Odyssey orbiter, which sees in both infrared and visible light wavelengths, discovered that the spots are nearly as cold as the carbon dioxide ice, suggesting they were just a thin layer of dark material lying on top of the ice and kept chilled by it. The morphology of these formations appears to be controlled by bedding and local jointing of the rocks; implying that expelled fluids are derived from within a few hundred meters of the surface. Some spider ravines modify, some destroy and others create crust in a dynamic near-surface process that extensively reworks the terrain creating and destroying surface layers. This process is rapid, happening in the space of a few days, weeks or months.

See also

References

  1. Kereszturi, A., ed. (2009), "POSSIBLE LIQUID-LIKE WATER PRODUCED SEEPAGE FEATURES ON MARS." (PDF), 40th. Lunar and Planetary Science Conference (2009), retrieved 2009-08-12 {{citation}}: |format= requires |url= (help); Cite has empty unknown parameter: |coauthors= (help); Unknown parameter |coeditors= ignored (help)
  2. ^ "NASA Findings Suggest Jets Bursting From Martian Ice Cap". Jet Propulsion Laboratory. NASA. August 16, 2006. Retrieved 2009-08-11. {{cite news}}: Cite has empty unknown parameter: |coauthors= (help)
  3. ^ Bérczi, Sz., ed. (2004), "STRATIGRAPHY OF SPECIAL LAYERS – TRANSIENT ONES ON PERMEABLE ONES: EXAMPLES" (PDF), Lunar and Planetary Science XXXV (2004), retrieved 2009-08-12 {{citation}}: |format= requires |url= (help); Cite has empty unknown parameter: |coauthors= (help); Unknown parameter |coeditors= ignored (help)
  4. ^ "Spiders on Earth and Mars (pp. 21)" (PDF). Australian Institute of Geoscientists. August 2006. Retrieved 2009-08-11.
  5. Photographic examples: 1, 2, 3
  6. ^ "SIMULATIONS OF GEYSER-TYPE ERUPTIONS IN CRYPTIC REGION OF MARTIAN SOUTH" (PDF), Fourth Mars Polar Science Conference, 2006, retrieved 2009-08-11 {{citation}}: |editor-first= missing |editor-last= (help); |format= requires |url= (help); Cite has empty unknown parameters: |coeditors= and |coauthors= (help)
  7. Spiders: Water-Driven Erosive Structures in the Southern Hemisphere of Mars. Prieto-Ballesteros, Olga et al. Astrobiology. August 2006, Vol. 6, No. 4. pp: 651-667
  8. Prieto-Ballesteros, Olga (2005). "Martian Spiders as feasible water-driven erosive structures" (PDF). Centro de Astrobiología-INTA-CSIC. Retrieved 2009-08-11. {{cite journal}}: Cite has empty unknown parameter: |coauthors= (help)
  9. [http://spsr.utsi.edu/articles/ness.pdf Peter K Ness and Greg M Orme. Spider-Ravine Models and Plant-like Features on Mars - Possible Geophysical and Biogeophysical Modes of Origin and Planet-like Features on Mars JBIS, Vol. 55, pp.85-108.]

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