Difference between revisions of "Rivers on Mars"

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Another type of channel exists mostly in the old, southern highlands.  They were discovered by Mariner 9 in 1971.  Sometimes called valley networks, these channels closely resemble streams in drainage basins on the Earth.  The channels are branched (dendritic).  However, branches are typically shorter on Mars than on the Earth. <ref> Baker, V. , and J. Partridge.  1986.  Small Martian valleys: Pristine and degraded morphology, J. Geophys. Res., 91, 3561–3572.</ref>  Also, most channels do not exhibit a high branching density.  But, in some places the stream branches are, in fact,  as dense as some on Earth.<ref> Hynek, B.M., and Phillips, R.  2001.  Evidence of extensive denudation of the martian highlands, Geology, 29, 407-10</ref>    Many look as if they were made with precipitation.  Further support for abundant water flow, came from a research team that developed a computer program to look for valleys made by streams found that the stream networks were much longer than previous thought (2.3 times longer) and that they were much denser.  Valleys were especially dense in northern Terra Cimmeria and the Margaritifer Terra.  There results suggest that precipitation may have caused them.<ref>https://www.astrobio.net/mars/martian-north-once-covered-by-ocean/</ref> <ref>Luo, W., T. Stepinski.  2009.  Computer‐generated global map of valley networks on Mars.  Journal of Geophysical Research: Planets:  114, Issue E11.  https://doi.org/10.1029/2009JE003357.</ref> <ref>https://agupubs.onlinelibrary.wiley.com/doi/full/10.1029/2009JE003357</ref>
 
Another type of channel exists mostly in the old, southern highlands.  They were discovered by Mariner 9 in 1971.  Sometimes called valley networks, these channels closely resemble streams in drainage basins on the Earth.  The channels are branched (dendritic).  However, branches are typically shorter on Mars than on the Earth. <ref> Baker, V. , and J. Partridge.  1986.  Small Martian valleys: Pristine and degraded morphology, J. Geophys. Res., 91, 3561–3572.</ref>  Also, most channels do not exhibit a high branching density.  But, in some places the stream branches are, in fact,  as dense as some on Earth.<ref> Hynek, B.M., and Phillips, R.  2001.  Evidence of extensive denudation of the martian highlands, Geology, 29, 407-10</ref>    Many look as if they were made with precipitation.  Further support for abundant water flow, came from a research team that developed a computer program to look for valleys made by streams found that the stream networks were much longer than previous thought (2.3 times longer) and that they were much denser.  Valleys were especially dense in northern Terra Cimmeria and the Margaritifer Terra.  There results suggest that precipitation may have caused them.<ref>https://www.astrobio.net/mars/martian-north-once-covered-by-ocean/</ref> <ref>Luo, W., T. Stepinski.  2009.  Computer‐generated global map of valley networks on Mars.  Journal of Geophysical Research: Planets:  114, Issue E11.  https://doi.org/10.1029/2009JE003357.</ref> <ref>https://agupubs.onlinelibrary.wiley.com/doi/full/10.1029/2009JE003357</ref>
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[[File:Warrego-Valles-system-located-at-422S-930W-The-drainage-density-of-this-Noachian.png|600pxr|Warrego Valles system as seen by the  Thermal Emission Imaging System on the Mars Odyssey spacecraft]]
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Warrego Valles system as seen by the  Thermal Emission Imaging System on the Mars Odyssey spacecraft
  
  

Revision as of 14:24, 21 April 2023

Mars topography (MOLA dataset) HiRes (1).jpg

Article written by Jim Secosky. Jim is a retired science teacher who has used the Hubble Space Telescope, the Mars Global Surveyor, and HiRISE.


Nirgal Vallis, as seen by Mariner 9 This is one of the first images to show evidence of past water on Mars.

There is much evidence that water once flowed in river valleys on Mars. Images of curved and branched channels have been seen in images from Mars spacecraft dating back to the early seventies with the Mariner 9 orbiter. [1] [2] [3] [4] [5] [6] These river valleys are called Vallis (plural Valles), the Latin word for valley.

Outflow Channels

Water poured out of the ground here at Ravi Vallis and carved a channel.


Researchers have grouped Martian river valleys into two groups. One type, called outflow channels, carried as much as or more water any on Earth and maybe at any time in Earth’s history.[7] Rushing water formed large streamlined islands. Vast quantities of water seem to have just burst out of the ground.[8] [9] [10] [11] [12] The water originated in areas of collapsed terrain where the ground ended up formed into mesas and large blocks. This collapsed terrain has been called chaos.[13] The water is thought to have flowed to lower elevations and created an ocean to the north that may have been one third the area of Mars.[14] [15] Some researches postulated that floods erupted from the ground many times.[16] [17] Since Mars is very cold, ice would have quickly formed on the top and allowed the water to move along for some time. Scientists generally agree that Mars has a thick shell of ice under the surface.[18] Perhaps in the past there was a vast interconnected layer of water under it. If an asteroid, fault, or volcanic eruption caused the ice to break, water could pour out. [19] [20] [21]


  • Labeled topo map of Kasei Valles and many other outflow channels These channels supplied water to a vast Martian Ocean.

  • Labeled topo map of outflow channels in the Oxia Palus region

  • Teardrop-shaped islands formed from water.

  • Maja Valles, an outflow channel, shaped land around Dromore crater.

  • Streamlined forms in wide channel These were shaped by running water.

Valley Networks

Another type of channel exists mostly in the old, southern highlands. They were discovered by Mariner 9 in 1971. Sometimes called valley networks, these channels closely resemble streams in drainage basins on the Earth. The channels are branched (dendritic). However, branches are typically shorter on Mars than on the Earth. [22] Also, most channels do not exhibit a high branching density. But, in some places the stream branches are, in fact, as dense as some on Earth.[23] Many look as if they were made with precipitation. Further support for abundant water flow, came from a research team that developed a computer program to look for valleys made by streams found that the stream networks were much longer than previous thought (2.3 times longer) and that they were much denser. Valleys were especially dense in northern Terra Cimmeria and the Margaritifer Terra. There results suggest that precipitation may have caused them.[24] [25] [26]

Warrego Valles system as seen by the Thermal Emission Imaging System on the Mars Odyssey spacecraft

Warrego Valles system as seen by the Thermal Emission Imaging System on the Mars Odyssey spacecraft


  • These branched channels, as seen by Viking look like they were caused by rainfall.

  • Small branched channel

  • Branched channel, as seen by HiRISE under HiWish Program

  • Channel network

Channels displaying curves, wide meanders, oxbow lakes, and wide meanders are similar to those on Earth. Many channels end in low areas such as craters. At times, deltas form where the stream enters a crater; they look like a stream entering a lake. Some small streams are found on valley floors. Stream channels on valley floors imply more than one episode of flow.[27] [28]


  • Small channel on floor of a valley suggest water flowed more than once here.

  • Channel on floor of a valley Water may have carved large valley early on; later the small channel was made.

  • Channels carried water in and out of craters.

  • Delta on Holden Crater floor, as seen by CTX

  • Channel in the Sinus Sabaeus quadrangle

  • An oxbow means that water flowed long enough to make a meander before the stream made a shortcut across the meanders.

  • Cutoff from a meander. This type of formations takes a long time to form.


Even though some channels go for relative short distances, some may run for hundreds or thousands of kilometers. One long system of lakes and rivers may reach from the far south to the far north. [29] [30] [31] In a study released in 2018, researchers found 34 palelakes and associated channels in the northeastern Hellas Basin. Because some were close to the Hadriacus volcano, some channels may have been created by hydrothermal systems; thereby allowing ice to melt. A number look as if they were formed from precipitation, others from groundwater.[32] [33] [34]

  • Curved and branched channels

Was Mars too cold for running water?

It seems that these valley networks happened in the past when Mars was much warmer and wetter. But, climate models all say that Mars was always too cold to have much liquid water. The sun is too far away. It likely did not give off as much light energy in the past.[35] [36] [37] Another factor that could still have made the climate warmer is that the atmosphere may have been much thicker in the past and could have contained greenhouse gases like carbon dioxide. However, if this were the case, carbon dioxide would have ended up in large deposits of carbonate rocks such as limestone.[38] Despite looking with instruments designed to detect carbonates, scientists have found very little. [39] They do exist in tiny areas, have been found in meteorites that came from Mars, and have been found by landers, but there just does not seem to be enough to say that Mars once had a thick carbon dioxide atmosphere. [40] [41] [42] [43] [44] Some researchers have proposed that other greenhouse gases may have been involved.[45] [46] So we are left with what appears to be certain proof that Mars had great amounts of liquid water—somehow channels were made. On the other hand, we do not know how the climate could have ever supported very much liquid water.[47] Nevertheless, scientists have suggested many ways for channels to be created. We must keep in mind that the planet does not have to that warmed to 32 degrees F for running water to exist because water on Mars would likely contain dissolved minerals that would lower its freezing point.[48] Also, water may have collected in vast aquifers under the ground and released at different times by things such as heating from magma moving underground or by impacts of asteroids. After large impacts, the nearby area might be warm enough, long enough for water to erode channels.[49] [50] [51] [52] [53] [54] [55] [56] It has even been suggested that the weather after a big impact may be changed enough to generate rainfall.[57] [58] [59] Some researchers think that streams may have existed under thick ice sheets. [60] [61] [62] [63] [64] [65] As of today, we just do not have a definite answer.

References

  1. ↑ Baker, V. 1982. The Channels of Mars. Univ. of Tex. Press, Austin, TX
  2. ↑ Baker, V., R. Strom, R., V. Gulick, J. Kargel, G. Komatsu, V. Kale. 1991. Ancient oceans, ice sheets and the hydrological cycle on Mars. Nature 352, 589–594.
  3. ↑ Carr, M. 1979. Formation of Martian flood features by release of water from confined aquifers. J. Geophys. Res. 84, 2995–300.
  4. ↑ Komar, P. 1979. Comparisons of the hydraulics of water flows in Martian outflow channels with flows of similar scale on Earth. Icarus 37, 156–181.
  5. ↑ http://advances.sciencemag.org/content/5/3/eaav7710
  6. ↑ Kite, E., et al. 2019. Persistence of intense, climate-driven runoff late in Mars history. Science Advances: 5, eaav7710
  7. ↑ https://www.uahirise.org/ESP_045833_1845
  8. ↑ Baker, V.R. (1982). The Channels of Mars. Austin: Texas University Press.
  9. ↑ Carr, M. (1979). "Formation of Martian flood features by release of water from confined aquifers". J. Geophys. Res., 84, 2995-3007.
  10. ↑ Clifford, S. M.; Parker, T. J. (2001). "The Evolution of the Martian Hydrosphere: Implications for the Fate of a Primordial Ocean and the Current State of the Northern Plains". Icarus. 154 (1): 40–79. Bibcode:2001Icar..154...40C. doi:10.1006/icar.2001.6671
  11. ↑ Andrews-Hanna, J., R. Phillips. 2007. Hydrological modeling of outflow channels and chaos regions on Mars. Journal of Geophysical Research: Planets Volume 112, Issue E8
  12. ↑ Clifford, S. 1993. A model for the hydrologic and climatic behavior of water on Mars. JGR, 98, 10973L
  13. ↑ Carr, M.H. (2006), The Surface of Mars. Cambridge Planetary Science Series, Cambridge University Press.
  14. ↑ https://www.sciencedaily.com/releases/2010/06/100613181245.htm
  15. ↑ Gaetano Di Achille, Brian M. Hynek. Ancient ocean on Mars supported by global distribution of deltas and valleys. Nature, 2010; DOI: 10.1038/ngeo891
  16. ↑ Coleman, N and C. Coughenour. 2021. CONSIDERATION OF STREAM POWER AND THE OUTFLOW CHANNELS OF MARS. 52nd Lunar and Planetary Science Conference 2021 (LPI Contrib. No. 2548). 1010.pdf
  17. ↑ Coleman N. (2010) LPSC 41, Abs. #1174, Kasei cataracts, https://www.lpi.usra.edu/meetings/lpsc2010/pdf/1174.pdf.
  18. ↑ Clifford, S. 1993. A model for the hydrologic and climatic behavior of water on Mars. Geophys. Res. 98 (E6)
  19. ↑ Carr, M. 1979. Formation of martian flood features by release of water from confined aquifers. J. Geophys. Res. 84: 2995-3007.
  20. ↑ ISBN 978-0-521-87501-0 Please check ISBN|reason=Check digit (0) does not correspond to calculated figure.
  21. ↑ Hanna, J. and R. Phillips. 2005. Tectonic pressurization of aquifers in the formation of Mangala and Athabasca Valles on Mars. LPSC XXXVI. Abstract 2261.
  22. ↑ Baker, V. , and J. Partridge. 1986. Small Martian valleys: Pristine and degraded morphology, J. Geophys. Res., 91, 3561–3572.
  23. ↑ Hynek, B.M., and Phillips, R. 2001. Evidence of extensive denudation of the martian highlands, Geology, 29, 407-10
  24. ↑ https://www.astrobio.net/mars/martian-north-once-covered-by-ocean/
  25. ↑ Luo, W., T. Stepinski. 2009. Computer‐generated global map of valley networks on Mars. Journal of Geophysical Research: Planets: 114, Issue E11. https://doi.org/10.1029/2009JE003357.
  26. ↑ https://agupubs.onlinelibrary.wiley.com/doi/full/10.1029/2009JE003357
  27. ↑ Malin, M.C., and Carr, M.H. (1999), Groundwater formation of martian valleys, Nature, 397, 589-592
  28. ↑ Jaumann, R. (2005), Martian valley networks and associated fluvial features as seen by the Mars Express High Resolution Camera (HRSC), LPSC XXXVI, Abstract 1815
  29. ↑ Cabrol, N., E. Grin. 1999. Distribution, classification, and ages of martian impact crater lakes. Icarus: 142, 160-172.
  30. ↑ Irwin, R.; et al. (2005). "An intense terminal epoch of widespread fluvial activity on early Mars. 2. Increased runoff and paleolake development". J. Geophys. Res. 110.
  31. ↑ Fassett, C.; Head, J. (2008). "Valley network-fed, open-basin lakes on Mars: Distribution and implications for Noachian surface and subsurface hydrology". Icarus. 198: 37–56.
  32. ↑ https://www.liebertpub.com/doi/abs/10.1089/ast.2018.1816?journalCode=ast
  33. ↑ https://www.seti.org/groundwater-and-precipitation-provided-water-form-lakes-along-northern-rim-hellas-basin-throughout
  34. ↑ Hargitai, H., et al. 2018. Groundwater-Fed, and Fluvial Lakes in the Navua–Hadriacus–Ausonia Region, Mars. Astrobiology: 18. (11). https://doi.org/10.1089/ast.2018.1816
  35. ↑ Wordsworth, R., et al. 2015. Comparison of “warm and wet” and “cold and icy” scenarios for early Mars in a 3‐D climate model. Journal of Geophysical Research: Planets Volume 120, Issue 6. https://doi.org/10.1002/2015JE004787.
  36. ↑ Squyres, S., J. Kasting. 1994. Early Mars: How Warm and How Wet? Science : Vol. 265, Issue 5173, pp. 744-749.
  37. ↑ Catling, D. C. (2007). Mars: Ancient fingerprints in the clay. Nature. 448 (7149): 31–32.
  38. ↑ http://www.psrd.hawaii.edu/Oct03/carbonatesMars.html
  39. ↑ Murchie, S., et al. 2009. A synthesis of Martian aqueous mineralogy after 1 Mars years of observations from the Mars Reconnaissance Orbiter. Journal of Geophysical Research: 114, E00D06
  40. ↑ McKay, C., et al. 1996. Search for Past Life on Mars: Possible Relic Biogenic Activity in Martian Meteorite ALH84001. Science: 273, 924-930
  41. ↑ https://www.webelements.com/nexus/carbonate-minerals-on-mars/
  42. ↑ https://mars.nasa.gov/mer/newsroom/pressreleases/20040109a.html
  43. ↑ Pollack, J. B, Roush, T., Witteborn, F., Bregman, J., Wooden, D., Stoker, C., Toon, O. B., Rank, D., Dalton, B., and Freedman, R. (1990) Thermal emission spectra of Mars (5.4-10.5 microns): evidence for sulfates, carbonates, and hydrates, Journal of Geophysical Research, v. 95 (B9), p. 14595-14627.
  44. ↑ https://mars.nasa.gov/resources/4040/carbonate-containing-martian-rocks/
  45. ↑ Ramirez, R. M., Kopparapu, R., Zugger, M. E., Robinson, T. D., Freedman, R., & Kasting, J. F. 2014. Warming early Mars with CO2 and H2. Nature Geoscience, 7(1), 59-63.
  46. ↑ Wordsworth, R., Kalugina, Y., Lokshtanov, S., Vigasin, A., Ehlmann, B., Head, J., ... & Wang, H. 2017. Transient reducing greenhouse warming on early Mars. Geophysical Research Letters, 44(2), 665-671.
  47. ↑ Haberle, R.M. 1998. Early Climate Models, J. Geophys. Res., 103(E12), 28467-79.
  48. ↑ Fairen, A., et al. 2009. Stability against freezing of aqueous solutions on early Mars. Nature: 459, 401-404
  49. ↑ https://www.hou.usra.edu/meetings/lpsc2019/pdf/2024.pdf
  50. ↑ Palumbo, A., J. Head. OCEANS ON MARS: THE POSSIBILITY OF A NOACHIAN GROUNDWATER-FED OCEAN IN A SUBFREEZING MARTIAN CLIMATE. 50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132). 2024.pdf
  51. ↑ Newsome, H.E. (1980), Hydrothermal alteration of impact melt sheets with implications for Mars, Icarus, 44, 207-16.
  52. ↑ Mangold, N., V. Ansan, P. Masson, C. Quantin, and G. Neukum. 2008. Geomorphic study of fluvial landforms on the northern Valles Marinerisplateau, Mars, J. Geophys. Res., 113, E08009, doi:10.1029/2007JE002985.
  53. ↑ Segura, T. L., O. B. Toon, and T. Colaprete. 2008. Modeling the environmentaleffects of moderate‐sized impacts on Mars, J. Geophys. Res., 113,E11007, doi:10.1029/2008JE003147
  54. ↑ Segura, T. L., O. B. Toon, T. Colaprete, and K. Zahnle. 2002. Environmental Effects of Large Impacts on Mars, Science, 298, 1977–1980. doi:10.1126/science.1073586
  55. ↑ Kraal, E. R., M. van Dijk, G. Postma, and M. G. Kleinhans 2008b. Martian stepped‐delta formation by rapid water release, Nature, 451. 973–976, doi:10.1038/nature06615
  56. ↑ Toon, O. B., T. Segura, and K. Zahnle. 2010. The formation of Martian river valleys by impacts, Annu. Rev. Earth Planet. Sci., 38, 303–322. doi:10.1146/annurev-earth-040809-152354
  57. ↑ https://arxiv.org/abs/1902.07666
  58. ↑ Turbet, M., et al. 2019. The environmental effects of very large bolide impacts on early Mars explored with a hierarchy of numerical models. Submitted to Icarus
  59. ↑ https://www.space.com/mars-water-from-massive-impacts.html?utm_source=sdc-newsletter&utm_medium=email&utm_campaign=20190305-sdc
  60. ↑ https://www.hou.usra.edu/meetings/lpsc2019/pdf/2574.pdf
  61. ↑ Galofre, G., et al. 2019. DID MARTIAN VALLEY NETWORKS FORM UNDER ANCIENT ICE SHEETS? 50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132). 2574.pdf
  62. ↑ Squyres, S.W., and Kasting, J.F. 1994. Early Mars: How warm and how wet?, Science, 265, 744-8.
  63. ↑ https://www.iflscience.com/space/massive-ice-sheets-not-rivers-may-have-carved-ancient-valleys-on-mars/
  64. ↑ https://www.nature.com/articles/s41561-020-0618-x
  65. ↑ Galofre, A. et al. 2020. Valley formation on early Mars by subglacial and fluvial erosion. Nature Geoscience.

See Also

External links

  • Head, J., et al. 2023. GEOLOGICAL AND CLIMATE HISTORY OF MARS: IDENTIFICATION OF POTENTIAL WARM AND

WET CLIMATE ‘FALSE POSITIVES’. 54th Lunar and Planetary Science Conference 2023 (LPI Contrib. No. 2806). 1731.pdf

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