Astronomy:Tharsis quadrangle

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Short description: Map of Mars
Tharsis quadrangle
USGS-Mars-MC-9-TharsisRegion-mola.png
Map of Tharsis quadrangle from Mars Orbiter Laser Altimeter (MOLA) data. The highest elevations are white and the lowest are blue.
Coordinates [ ⚑ ] : 15°00′N 112°30′W / 15°N 112.5°W / 15; -112.5
Image of the Tharsis Quadrangle (MC-9). The region contains the Olympus Mons, Ascraeus Mons and Pavonis Mons, three of the four largest shield volanoes on Mars. The north-central part contains Ceraunius Fossae.

The Tharsis quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS) Astrogeology Research Program. The Tharsis quadrangle is also referred to as MC-9 (Mars Chart-9).[1] The name Tharsis refers to a land mentioned in the Bible. It may be at the location of the old town of Tartessus at the mouth of Guadalquivir.[2]

Main page: Astronomy:Classical albedo features on Mars

The quadrangle covers the area from 90° to 135° west longitude and 0° to 30° north latitude on Mars and contains most of the Tharsis Rise. The plateau is about as high as Earth's Mount Everest and about as big in area as all of Europe. Tharsis contains a group of large volcanoes. Olympus Mons is the tallest.[3]

Within the quadrangle, the two largest impact craters are Poynting and Paros.

Volcanoes

Main page: Astronomy:Volcanology of Mars

Tharsis is a land of great volcanoes. Olympus Mons is the tallest known volcano in the Solar System; it is 100 times larger than any volcano on Earth. Ascraeus Mons and Pavonis Mons are at least 200 miles across and are over six miles above the plateau that they sit on—and, the plateau is three to four miles above the zero altitude of Mars.[4] Pavonis Mons, the middle in a line of three volcanoes, sits at just about dead center on the equator. Mons is a term used for a large raised feature. Tholus is about the same, but smaller. A patera is flatter and like a volcano with a super large opening. Actually, a patera is formed when the top of a volcano collapses because its magma chamber is empty. Crater Lake Oregon was formed that way. Several volcanoes form a straight line in the Tharsis Uplift. Two major ones are in the Tharsus quadrangle: Ascraeus Mons and Pavonis Mons. It has been proposed that these are the result of plate motion which on Earth makes volcanic arc islands.[5][6][7][8][9]

Although Mars displays many volcanoes here and other places, there has been no evidence of recent volcanic activity, even at a very low level. Research, published in 2017, found no active release of volcanic gases during two successive Martian years. They looked for the outgassing of sulfur-bearing chemicals with spectrometers.[10]

Images

Potential influence of volcanic emissions on climate

Some scientists maintain that Tharsis has had great influence on the climate of Mars. Volcanoes give off large amounts of gas when they erupt. The gases are usually water vapor and carbon dioxide. Some estimates put the amount of gas released to the atmosphere as enough to make the atmosphere thicker than the Earth's. In addition, the water released by the volcanoes could have been enough to cover all of Mars to a depth of 120 meters. The greenhouse effect of carbon dioxide raises the temperature of a planet by trapping heat in the form of infrared radiation. The volcanic eruptions on Tharsis could have made Mars more Earth-like in the past. Mars may have once had a much thicker and warmer atmosphere. Oceans and/or lakes may have been present.[3]

Fossa

The Tharsis quadrangle is also home to large troughs (long narrow depressions) called fossae in the geographical language used for Mars. Fossae in this area are Ulysses Fossae, Olympica Fossae, Ceraunius Fossae, and Tractus Fossae. These troughs form when the crust is stretched until it breaks. The stretching can be due to the large weight of a nearby volcano. Studies have shown that the volcanoes of Tharsis caused most of the major fossae on Mars. The stress that caused the fossae and other tectonic features is centered in Noctis Labyrinthus, at 4 S and 253 E. But the center has moved somewhat over time.[11][12] Fossae/pit craters are common near volcanoes in the Tharsis and Elysium system of volcanoes.[13] A trough often has two breaks with a middle section moving down, leaving steep cliffs along the sides; such a trough is called a graben.[14] Studies have found that on Mars a fault may be as deep as 5 km, that is the break in the rock goes down to 5 km. Moreover, the crack or fault sometimes widens or dilates. This widening causes a void to form with a relatively high volume. When material slides into the void, a pit crater or a pit crater chain forms. Pit craters do not have rims or ejecta around them, like impact craters do. On Mars, individual pit craters can join to form chains or even to form troughs that are sometimes scalloped.[15] Other ideas have been suggested for the formation of fossae and pit craters. There is evidence that they are associated with dikes of magma. Magma might move along, under the surface, breaking the rock and, more importantly, melting ice. The resulting action would cause a crack to form at the surface. Pit craters are not common on Earth. Sinkholes, where the ground falls into a hole (sometimes in the middle of a town) resemble pit craters on Mars. However, on the Earth these holes are caused by limestone being dissolved thereby causing a void.[15][16][17]

Knowledge of the locations and formation mechanisms of pit craters and fossae is important for the future colonization of Mars because they may be reservoirs of water.[18]

  • Ulysses Fossae mound, as seen by HiRISE.

  • Ceraunius Fossae, as seen by HiRISE.

  • Olympica Fossae, as seen by HiRISE. Click on image to see rock layers in wall.

  • Trough in Tractus Fossae caused by faults and resulting collapse of material into faults forming a chain of pits, as seen by Mars Global Surveyor.

  • Tractus Fossae Ringed Pit, as seen by HiRISE. Scale bar is 1000 meters long.

  • Pits and troughs with layers, as seen by HiRISE under HiWish program

  • Line of pits turning into a trough, as seen by HiRISE under HiWish program

  • Fossae, as seen by HiRISE under HiWish program

  • Troughs and channels, as seen by HiRISE under HiWish program

Glaciers

Main page: Astronomy:Glaciers on Mars

Some scientists see evidence that glaciers exist on many of the volcanoes in Tharsis, including Olympus Mons, Ascraeus Mons, and Pavonis Mons.[11][19][20] Ceraunius Tholus may have even had its glaciers melt to form some temporary lakes in the past.[21][22][23][24][25][26][27]

Ice sheet

Tharsis may have been the location for a giant ice sheet.[28] [29] [30] [31] [32] It would have been in the Late Hesperian time period. It may have melted quickly due to events like volcanism or impacts and it could have contributed to a northern ocean.[33] [34] [35] [36] Some researchers have suggested that lava flows covered the ice cap, thereby causing it to melt rather quickly. The water could have created the outflow channels around Tharsis.[37]

Dark slope streaks

Some pictures below show dark streaks: on the slopes on large blocks just to the left of Tharsis Tholus, on Ceraunius Fossae, and on Olympica Fossae. Such streaks are common on Mars. They occur on steep slopes of craters, troughs, and valleys. The streaks are dark at first. They get lighter with age.[38] Sometimes they start in a tiny spot, then spread out and go for hundreds of meters. They have been seen to travel around obstacles, like boulders.[39] It is believed that they are avalanches of bright dust that expose a darker underlying layer. However, several ideas have been advanced to explain them. Some involve water or even the growth of organisms.[40][41][42] The streaks appear in areas covered with dust. Much of the Martian surface is covered with dust. Fine dust settles out of the atmosphere covering everything. We know a lot about it because the solar panels of the Mars Rovers get covered with it, thus reducing the electrical energy. The power of the Rovers has been restored many times by the wind, in the form of dust devils, clearing the panels and thus boosting the power.[43] Dust storms are frequent, especially when the spring season begins in the southern hemisphere. At that time, Mars is 40% closer to the sun. The orbit of Mars is much more elliptical then the Earth's. That is the difference between the farthest point from the sun and the closest point to the sun is very great for Mars, but only a slight amount for the Earth. Also, every few years, the entire planet is engulfed in global dust storms. When NASA's Mariner 9 craft arrived there, nothing could be seen through the dust storm.[44][45] Other global dust storms have also been observed, since that time.

  • Sulci Gordii Terraced Hills, as seen by HiRISE. Many dark slope streaks are visible.

  • Ceraunius Tholus Channel, as seen by HiRISE. The summit crater of Ceraunius Tholus is just to the right of this picture. Click on image to see dark slope streaks. The scale bar is 1000 meters long. Straight dark lines are where no data were collected.

  • ESP 054980 2040streaks.jpg

Research, published in January 2012 in Icarus, found that dark streaks were initiated by airblasts from meteorites traveling at supersonic speeds. The team of scientists was led by Kaylan Burleigh, an undergraduate at the University of Arizona. After counting some 65,000 dark streaks around the impact site of a group of 5 new craters, patterns emerged. The number of streaks was greatest closer to the impact site. So, the impact somehow probably caused the streaks. Also, the distribution of the streaks formed a pattern with two wings extending from the impact site. The curved wings resembled scimitars, curved knives. This pattern suggests that an interaction of airblasts from the group of meteorites shook dust loose enough to start dust avalanches that formed the many dark streaks. At first it was thought that the shaking of the ground from the impact caused the dust avalanches, but if that was the case the dark streaks would have been arranged symmetrically around the impacts, rather than being concentrated into curved shapes.

The crater cluster lies near the equator 510 miles) south of Olympus Mons, on a type of terrain called the Medusae Fossae formation. The formation is coated with dust and contains wind-carved ridges called yardangs. These yardangs have steep slopes thickly covered with dust, so when the sonic boom of the airblast arrived from the impacts dust started to move down the slope. Using photos from Mars Global Surveyor and HiRISE camera on NASA’s Mars Reconnaissance Orbiter, scientists have found about 20 new impacts each year on Mars. Because the spacecraft have been imaging Mars almost continuously for a span of 14 years, newer images with suspected recent craters can be compared to older images to determine when the craters were formed. Since the craters were spotted in a HiRISE image from February 2006, but were not present in a Mars Global Surveyor image taken in May 2004, the impact occurred in that time frame.

The largest crater in the cluster is about 22 meters (72 feet) in diameter with close to the area of a basketball court. As the meteorite traveled through the Martian atmosphere it probably broke up; hence a tight group of impact craters resulted. Dark slope streaks have been seen for some time, and many ideas have been advanced to explain them. This research may have finally solved this mystery.[46][47]

  • Image indicates crater cluster and curved lines formed by airblast from meteorites. Meteorites caused airblast which caused dust avalanches on steep slopes. Image is from HiRISE.

  • Close-up of previous image along light/dark boundary. Dark line in middle of image shows border between light and dark area of curved lines. Green arrows show high areas of ridges. Loose dust moved down steep slopes when it felt the airblast from meteorite strikes. Image is from HiRISE.

Lava flows

  • Lava flows in the Tharsis quadrangle.

  • Lava flow in Tharsis quadrangle, as seen by HiRISE under HiWish program

  • Close-up of lava flow with labels, as seen by HiRISE under HiWish program Note: this is an enlargement of the previous image of lava flows.

  • Image shows both young and old lava flows from the base of Olympus Mons. The flat plain is the younger flow. The older flow has channels with levees along their edges. The presence of levees is quite common in many lava flows.

  • Lava flows with older and younger flows labeled, as seen by HiRISE under HiWish program

  • Wide view of lava flowing over cliff around Olympus Mons, as seen by CTX

  • Close view of lava moving over cliff around Olympus Mons, as seen by HiRISE under HiWish program

Other features in the Tharsis quadrangle

  • Tharsis Tholus block, as seen by HiRISE. Block probably tumbled down Tharsis Tholus which is just off to the right.

  • Pangboche Crater, as seen by HiRISE. Pangboche Crater is a very young 11 km diameter crater near the summit of Olympus Mons. Notice the steep walls.

  • Tractus Catena Floor, as seen by HiRISE. Scale bar is 500 meters long.

  • Gigas Sulci, as seen by THEMIS. Wavy linear ridges are dunes. Dark slope streaks are visible on some slopes if you click on image for larger view.

  • Rahe Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter).

  • Delta in Rahe Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter). Note: this is an enlargement from the previous image of Rahe Crater.

  • Flows and pits, as seen by HiRISE under HiWish program

Other Mars quadrangles

Mars Quad Map
Mars Quad Map
The image above contains clickable linksClickable image of the 30 cartographic quadrangles of Mars, defined by the USGS.[48][49] Quadrangle numbers (beginning with MC for "Mars Chart")[50] and names link to the corresponding articles. North is at the top; [ ⚑ ] 0°N 180°W / 0°N 180°W / 0; -180 is at the far left on the equator. The map images were taken by the Mars Global Surveyor.

Interactive Mars map

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See also


References

  1. ↑ Davies, M.E.; Batson, R.M.; Wu, S.S.C. (1992). "Geodesy and Cartography". in Kieffer, H.H.; Jakosky, B.M.; Snyder, C.W. et al.. Mars. Tucson: University of Arizona Press. ISBN 978-0-8165-1257-7. https://archive.org/details/mars0000unse. 
  2. ↑ Blunck, J. 1982. Mars and its Satellites. Exposition Press. Smithtown, N.Y.
  3. ↑ 3.0 3.1 Hartmann, W.K. (2003-01-01). A Traveller's Guide to Mars: The Mysterious Landscapes of the Red Planet. New York: Workman. p. [1] [page needed]. ISBN 978-0-7611-2606-5. https://archive.org/details/travelersguideto00will/page/. 
  4. ↑ Norton, O. 2002. Mapping Mars. Picador, New York.
  5. ↑ Bell, Jim (2008-06-05). The Martian Surface: Composition, Mineralogy and Physical Properties. Cambridge University Press. ISBN 978-0-521-86698-9. 
  6. ↑ Sleep, Norman H. (1994). "Martian plate tectonics". Journal of Geophysical Research 99 (E3): 5639–5655. doi:10.1029/94JE00216. Bibcode: 1994JGR....99.5639S. 
  7. ↑ Barlow, Nadine (2008-01-10). Mars: An Introduction to its Interior, Surface and Atmosphere. Cambridge University Press. ISBN 978-0-521-85226-5. 
  8. ↑ http://dsc.discovery.com/news/2008/12/16/mars-shell-tectonics.html
  9. ↑ Connerney, J. E. P.; Acuna, M. H.; Ness, N. F.; Kletetschka, G.; Mitchell, D. L.; Lin, R. P.; Reme, H. (2005). "Tectonic implications of Mars crustal magnetism". Proceedings of the National Academy of Sciences 102 (42): 14970–14975. doi:10.1073/pnas.0507469102. PMID 16217034. Bibcode: 2005PNAS..10214970C. 
  10. ↑ Khayat, A., et al. 2017. A deep search for the release of volcanic gases on Mars using ground-based high-resolution infrared and submillimeter spectroscopy: Sensitive upper limits for OCS and SO2. Icarus: 296, 1-14.
  11. ↑ 11.0 11.1 Carr, Michael H. (2006). The Surface of Mars. Cambridge University Press. p. [page needed]. ISBN 978-0-521-87201-0. 
  12. ↑ Anderson, Robert C.; Dohm, James M.; Golombek, Matthew P.; Haldemann, Albert F. C.; Franklin, Brenda J.; Tanaka, Kenneth L.; Lias, Juan; Peer, Brian (2001). "Primary centers and secondary concentrations of tectonic activity through time in the western hemisphere of Mars". Journal of Geophysical Research 106 (E9): 20563–20585. doi:10.1029/2000JE001278. Bibcode: 2001JGR...10620563A. 
  13. ↑ Skinner, J.; Skinner, L.; Kargel, J. (2007). "Re-assessment of Hydrovolcanism-based Resurfacing within the Galaxias Fossae Region of Mars". Lunar and Planetary Science XXXVIII (1338): 1998. Bibcode: 2007LPI....38.1998S. http://www.lpi.usra.edu/meetings/lpsc2007/pdf/1998.pdf. 
  14. ↑ "HiRISE | Craters and Pit Crater Chains in Chryse Planitia (PSP_008641_2105)". http://hirise.lpl.arizona.edu/PSP_008641_2105. 
  15. ↑ 15.0 15.1 Wyrick, D.; Ferrill, D.; Sims, D.; Colton, S. (2003). "Distribution, Morphology and Structural Associations of Martian Pit Crater Chains". Lunar and Planetary Science XXXIV: 2025. Bibcode: 2003LPI....34.2025W. 
  16. ↑ http://www.swri.edu/4org/d20/DEMPS/planetgeo/planetmars.html[no|permanent dead link|dead link}}]
  17. ↑ "Mars Global Surveyor MOC2-620 Release". http://www.msss.com/mars_images/moc/2004/01/29/index.html. 
  18. ↑ Ferrill, David A.; Wyrick, Danielle Y.; Morris, Alan P.; Sims, Darrell W.; Franklin, Nathan M. (2004). "Dilational fault slip and pit chain formation on Mars". GSA Today 14 (10): 4. doi:10.1130/1052-5173(2004)014<4:DFSAPC>2.0.CO;2. ISSN 1052-5173. https://www.geosociety.org/gsatoday/archive/14/10/pdf/i1052-5173-14-10-4.pdf. 
  19. ↑ http://www.lpi.edu/meetings/polar2003/pdf/8105.pdf[no|permanent dead link|dead link}}]
  20. ↑ Shean, David E. (2005). "Origin and evolution of cold-based tropical mountain glacier on Mars: the Pavonis Mons fan-shaped deposit". Journal of Geophysical Research 110 (E5). doi:10.1029/2004JE002360. Bibcode: 2005JGRE..110.5001S. 
  21. ↑ Fassett, C; Headiii, J (2007). "Valley formation on martian volcanoes in the Hesperian: Evidence for melting of summit snowpack, caldera lake formation, drainage and erosion on Ceraunius Tholus". Icarus 189 (1): 118–135. doi:10.1016/j.icarus.2006.12.021. Bibcode: 2007Icar..189..118F. http://www.planetary.brown.edu/pdfs/3408.pdf. 
  22. ↑ http://www.mars.asu/christensen/advancedmarsclass/shean_glaciers_2005.pdf[no|permanent dead link|dead link}}]
  23. ↑ Head, JW; Neukum, G; Jaumann, R; Hiesinger, H; Hauber, E; Carr, M; Masson, P; Foing, B et al. (2005). "Tropical to mid-latitude snow and ice accumulation, flow and glaciation on Mars". Nature 434 (7031): 346–350. doi:10.1038/nature03359. PMID 15772652. Bibcode: 2005Natur.434..346H. 
  24. ↑ http://www.marstoday.com/news/viewpr.html?pid=18050
  25. ↑ "Glaciers Reveal Martian Climate Has Been Recently Active". http://news.brown.edu/pressreleases/2008/04/martian-glaciers. 
  26. ↑ Plaut, Jeffrey J.; Safaeinili, Ali; Holt, John W.; Phillips, Roger J.; Head, James W.; Seu, Roberto; Putzig, Nathaniel E.; Frigeri, Alessandro (2009). "Radar Evidence for Ice in Lobate Debris Aprons in the Mid-Northern Latitudes of Mars". Geophysical Research Letters 36 (2): n/a. doi:10.1029/2008GL036379. Bibcode: 2009GeoRL..36.2203P. http://www.lpi.usra.edu/meetings/lpsc2008/pdf/2290.pdf. 
  27. ↑ Holt, J.W.; Safaeinili, A.; Plaut, J. J.; Young, D. A.; Head, J. W.; Phillips, R. J.; Campbell, B. A.; Carter, L. M. et al. (2008). "Radar Sounding Evidence for Ice within Lobate Debris Aprons near Hellas Basin, Mid-Southern Latitudes of Mars". Lunar and Planetary Science XXXIX (1391): 2441. Bibcode: 2008LPI....39.2441H. http://www.lpi.usra.edu/meetings/lpsc2008/pdf/2441.pdf. 
  28. ↑ Yin, An; Moon, Seulgi; Day, Mackenzie (2021). "Landform evolution of Oudemans crater and its bounding plateau plains on Mars: Geomorphological constraints on the Tharsis ice-cap hypothesis". Icarus 360. doi:10.1016/j.icarus.2021.114332. Bibcode: 2021Icar..36014332Y. https://www.sciencedirect.com/science/article/pii/S0019103521000300. 
  29. ↑ Lin, A., et al. 2023. Landform evolution of Oudemans crater and its bounding plateau plains on Mars: Geomorphological constraints on the Tharsis ice-cap hypothesis. Icarus. Volume 360, 15 May 2021, 114332
  30. ↑ V.R. Baker, R.G. Strom, J.M. Dohm, V.C. Gulick, J.S. Kargel, G. Komatsu, G.G. Ori, J.W. Rice Jr. Mars’ Oceanus Borealis, ancient glaciers, and the MEGAOUTFLO hypothesis. Lunar Planet. Sci, XXXI (2000), p. 1863
  31. ↑ K.P. Harrison, R.E. Grimm. 2004. Tharsis recharge: A source of groundwater for Martian outflow channels. Geophys. Res. Lett., 31 (14)
  32. ↑ J.P. Cassanelli, J.W. Head. 2019. Glaciovolcanism in the Tharsis volcanic province of Mars: Implications for regional geology and hydrology. Planet. Space Sci., 169. pp. 45-69
  33. ↑ B.K. Lucchitta Antarctic ice streams and outflow channels on Mars. Geophys. Res. Lett., 28 (3) (2001), pp. 403-406
  34. ↑ M.H. Carr, J.W. Head III. 2010. Geologic history of Mars Earth Planet. Sci. Lett., 294 (3–4). pp. 185-203
  35. ↑ M.H. Carr, J.W. Head. 2015. Martian surface/near-surface water inventory: Sources, sinks, and changes with time Geophys. Res. Lett., 42 (3). pp. 726-732
  36. ↑ M. Carr, J. Head. 2019. Mars: Formation and fate of a frozen Hesperian ocean. Icarus, 319. pp. 433-443
  37. ↑ J.P. Cassanelli, J.W. Head. 2019. Glaciovolcanism in the Tharsis volcanic province of Mars: Implications for regional geology and hydrology. Planet. Space Sci. pp. 45-69
  38. ↑ Schorghofer, N (2007). "Three decades of slope streak activity on Mars". Icarus 191 (1): 132–140. doi:10.1016/j.icarus.2007.04.026. Bibcode: 2007Icar..191..132S. 
  39. ↑ http://www.space.com/image_of_day_080730.html [|permanent dead link|dead link}}]
  40. ↑ "SPACE.com -- Dark Streaks on Mars Suggest Running Water Still Present". http://www.space.com/scienceastronomy/streaks_mars_021211.html. 
  41. ↑ http://www.space.com/scienceastronomy/streaks_mars_streaks_030328.html [|permanent dead link|dead link}}]
  42. ↑ http://www.space.com/scienceastronomy/mars_ [|permanent dead link|dead link}}]
  43. ↑ "Mars Spirit Rover Gets Energy Boost From Cleaner Solar Panels". ScienceDaily. February 19, 2009. https://www.sciencedaily.com/releases/2009/02/090217101110.htm. 
  44. ↑ Moore, Patrick (1990-06-02). Atlas of the Solar System. Crescent Books. ISBN 978-0-517-00192-9. https://archive.org/details/atlasofsolarsyst0000unse. 
  45. ↑ Kieffer, Hugh H. (1992). Mars. Tucson: University of Arizona Press. pp. [2] [page needed]. ISBN 978-0-8165-1257-7. https://archive.org/details/mars0000unse/page/. 
  46. ↑ Burleigh, Kaylan J.; Melosh, Henry J.; Tornabene, Livio L.; Ivanov, Boris; McEwen, Alfred S.; Daubar, Ingrid J. (2012). "Impact air blast triggers dust avalanches on Mars". Icarus 217 (1): 194–201. doi:10.1016/j.icarus.2011.10.026. Bibcode: 2012Icar..217..194B. 
  47. ↑ http://redplanet.asu.edu/
  48. ↑ Morton, Oliver (2002). Mapping Mars: Science, Imagination, and the Birth of a World. New York: Picador USA. p. 98. ISBN 0-312-24551-3. 
  49. ↑ "Online Atlas of Mars". http://ralphaeschliman.com/id30.htm. Retrieved December 16, 2012. 
  50. ↑ "PIA03467: The MGS MOC Wide Angle Map of Mars". NASA / Jet Propulsion Laboratory. February 16, 2002. http://photojournal.jpl.nasa.gov/catalog/PIA03467. Retrieved December 16, 2012. 

External links



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