Open main menu

The Phaethontis quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS) Astrogeology Research Program. The Phaethontis quadrangle is also referred to as MC-24 (Mars Chart-24).[1]

Phaethontis quadrangle
Map of Phaethontis quadrangle from Mars Orbiter Laser Altimeter (MOLA) data. The highest elevations are red and the lowest are blue.
Coordinates47°30′S 150°00′W﻿ / ﻿47.5°S 150°W﻿ / -47.5; -150Coordinates: 47°30′S 150°00′W﻿ / ﻿47.5°S 150°W﻿ / -47.5; -150
Image of the Phaethontis Quadrangle (MC-24). The region is dominated by heavily cratered highlands and low-lying areas forming relatively smooth plains.

The name comes from Phaethon, the son of Helios.[2]

The Phaethontis quadrangle lies between 30° and 65 ° south latitude and 120° and 180 ° west longitude on Mars. This latitude range is where numerous gullies have been discovered. An old feature in this area, called Terra Sirenum lies in this quadrangle; Mars Reconnaissance Orbiter discovered iron/magnesium smectites there.[3] Part of this quadrangle contains what is called the Electris deposits, a deposit that is 100–200 meters thick. It is light-toned and appears to be weak because of few boulders.[4] Among a group of large craters is Mariner Crater, first observed by the Mariner IV spacecraft in the summer of 1965. It was named after that spacecraft.[5] A low area in Terra Sirenum is believed to have once held a lake that eventually drained through Ma'adim Vallis.[6][7][8] Russia's Mars 3 probe landed in the Phaethontis quadrangle at 44.9° S and 160.1° W in December 1971. It landed at a speed of 75 km per hour, but survived to radio back 20 seconds of signal, then it went dead. Its message just appeared as a blank screen.[9]

Martian gulliesEdit

The Phaethontis quadrangle is the location of many gullies that may be due to recent flowing water. Some are found in the Gorgonum Chaos[10][11] and in many craters near the large craters Copernicus and Newton (Martian crater).[12][13] Gullies occur on steep slopes, especially on the walls of craters. Gullies are believed to be relatively young because they have few, if any craters. Moreover, they lie on top of sand dunes which themselves are considered to be quite young. Usually, each gully has an alcove, channel, and apron. Some studies have found that gullies occur on slopes that face all directions,[14] others have found that the greater number of gullies are found on poleward facing slopes, especially from 30-44 S.[15]

Although many ideas have been put forward to explain them,[16] the most popular involve liquid water coming from an aquifer, from melting at the base of old glaciers, or from the melting of ice in the ground when the climate was warmer.[17][18] Because of the good possibility that liquid water was involved with their formation and that they could be very young, scientists are excited. Maybe the gullies are where we should go to find life.


As for the next theory, much of the surface of Mars is covered by a thick smooth mantle that is thought to be a mixture of ice and dust.[21][22][23] This ice-rich mantle, a few yards thick, smoothes the land, but in places it has a bumpy texture, resembling the surface of a basketball. The mantle may be like a glacier and under certain conditions the ice that is mixed in the mantle could melt and flow down the slopes and make gullies.[24][25] Because there are few craters on this mantle, the mantle is relatively young. An excellent view of this mantle is shown below in the picture of the Ptolemaeus Crater Rim, as seen by HiRISE.[26] The ice-rich mantle may be the result of climate changes.[27] Changes in Mars's orbit and tilt cause significant changes in the distribution of water ice from polar regions down to latitudes equivalent to Texas. During certain climate periods water vapor leaves polar ice and enters the atmosphere. The water comes back to ground at lower latitudes as deposits of frost or snow mixed generously with dust. The atmosphere of Mars contains a great deal of fine dust particles. Water vapor will condense on the particles, then fall down to the ground due to the additional weight of the water coating. When Mars is at its greatest tilt or obliquity, up to 2 cm of ice could be removed from the summer ice cap and deposited at midlatitudes. This movement of water could last for several thousand years and create a snow layer of up to around 10 meters thick.[28][29] When ice at the top of the mantling layer goes back into the atmosphere, it leaves behind dust, which insulating the remaining ice.[30] Measurements of altitudes and slopes of gullies support the idea that snowpacks or glaciers are associated with gullies. Steeper slopes have more shade which would preserve snow.[15] Higher elevations have far fewer gullies because ice would tend to sublimate more in the thin air of the higher altitude.[31]

The third theory might be possible since climate changes may be enough to simply allow ice in the ground to melt and thus form the gullies. During a warmer climate, the first few meters of ground could thaw and produce a "debris flow" similar to those on the dry and cold Greenland east coast.[32] Since the gullies occur on steep slopes only a small decrease of the shear strength of the soil particles is needed to begin the flow. Small amounts of liquid water from melted ground ice could be enough.[33][34] Calculations show that a third of a mm of runoff can be produced each day for 50 days of each Martian year, even under current conditions.[35]

Associated features of gulliesEdit

Sometimes other features appear near gullies. At the base of some gullies there may be depressions or curved ridges. These have been called "spatulate depressions." These depressions form after glacial ice disappears. Steep walls often develop glaciers during certain climates. When the climate changes, the ice in the glaciers sublimates in the thin Martian atmosphere. Sublimation is when a substance goes directly from a solid state to a gas state. Dry ice on Earth does this. So when the ice at the base of a steep wall sublimates, a depression results. Also, more ice from higher up will tend to flow downward. This flow will stretch the surface rocky debris thereby forming transverse crevasses. Such formations have been termed "washboard terrain" because they resemble the old fashioned washboards.[36] The parts of gullies and some associated features of gullies are shown below in a HiRISE images.

Tongue-shaped glaciersEdit

Possible pingosEdit

The radial and concentric cracks visible here are common when forces penetrate a brittle layer, such as a rock thrown through a glass window. These particular fractures were probably created by something emerging from below the brittle Martian surface. Ice may have accumulated under the surface in a lens shape; thus making these cracked mounds. Ice being less dense than rock, pushed upwards on the surface and generated these spider web-like patterns. A similar process creates similar sized mounds in arctic tundra on Earth. Such features are called “pingos,”, an Inuit word.[37] Pingos would contain pure water ice; thus they could be sources of water for future colonists of Mars.

Concentric crater fillEdit

Concentric crater fill, like lobate debris aprons and lineated valley fill, is believed to be ice-rich.[38] Based on accurate topography measures of height at different points in these craters and calculations of how deep the craters should be based on their diameters, it is thought that the craters are 80% filled with mostly ice.[39][40][41][42] That is, they hold hundreds of meters of material that probably consists of ice with a few tens of meters of surface debris.[43][44] The ice accumulated in the crater from snowfall in previous climates.[45][46][47] Recent modeling suggests that concentric crater fill develops over many cycles in which snow is deposited, then moves into the crater. Once inside the crater shade and dust preserve the snow. The snow changes to ice. The many concentric lines are created by the many cycles of snow accumulation. Generally snow accumulates whenever the axial tilt reaches 35 degrees.[48]

Magnetic stripes and plate tectonicsEdit

The Mars Global Surveyor (MGS) discovered magnetic stripes in the crust of Mars, especially in the Phaethontis and Eridania quadrangles (Terra Cimmeria and Terra Sirenum).[49][50] The magnetometer on MGS discovered 100 km wide stripes of magnetized crust running roughly parallel for up to 2000 km. These stripes alternate in polarity with the north magnetic pole of one pointing up from the surface and the north magnetic pole of the next pointing down.[51] When similar stripes were discovered on Earth in the 1960s, they were taken as evidence of plate tectonics. Researchers believe these magnetic stripes on Mars are evidence for a short, early period of plate tectonic activity. When the rocks became solid they retained the magnetism that existed at the time. A magnetic field of a planet is believed to be caused by fluid motions under the surface.[52][53][54] However, there are some differences, between the magnetic stripes on Earth and those on Mars. The Martian stripes are wider, much more strongly magnetized, and do not appear to spread out from a middle crustal spreading zone. Because the area containing the magnetic stripes is about 4 billion years old, it is believed that the global magnetic field probably lasted for only the first few hundred million years of Mars' life, when the temperature of the molten iron in the planet's core might have been high enough to mix it into a magnetic dynamo. There are no magnetic fields near large impact basins like Hellas. The shock of the impact may have erased the remnant magnetization in the rock. So, magnetism produced by early fluid motion in the core would not have existed after the impacts.[55]

When molten rock containing magnetic material, such as hematite (Fe2O3), cools and solidifies in the presence of a magnetic field, it becomes magnetized and takes on the polarity of the background field. This magnetism is lost only if the rock is subsequently heated above a particular temperature (the Curie point which is 770 °C for iron). The magnetism left in rocks is a record of the magnetic field when the rock solidified.[56]

Chloride depositsEdit

Using data from Mars Global Surveyor, Mars Odyssey and the Mars Reconnaissance Orbiter, scientists have found widespread deposits of chloride minerals. A picture below shows some deposits within the Phaethontis quadrangle. Evidence suggests that the deposits were formed from the evaporation of mineral enriched waters. The research suggests that lakes may have been scattered over large areas of the Martian surface. Usually chlorides are the last minerals to come out of solution. Carbonates, sulfates, and silica should precipitate out ahead of them. Sulfates and silica have been found by the Mars Rovers on the surface. Places with chloride minerals may have once held various life forms. Furthermore, such areas should preserve traces of ancient life.[57]

Based on chloride deposits and hydrated phyllosilicates, Alfonso Davila and others believe there is an ancient lakebed in Terra Sirenum that had an area of 30,000 km2 and was 200 meters deep. Other evidence that supports this lake are normal and inverted channels like ones found in the Atacama desert.[58]


The Elysium quadrangle is home to large troughs (long narrow depressions) called fossae in the geographical language used for Mars. Troughs are created when the crust is stretched until it breaks. The stretching can be due to the large weight of a nearby volcano. Fossae/pit craters are common near volcanoes in the Tharsis and Elysium system of volcanoes.[59]

Strange surfacesEdit


Copernicus crater

The density of impact craters is used to determine the surface ages of Mars and other solar system bodies.[60] The older the surface, the more craters present. Crater shapes can reveal the presence of ground ice.

East side of Hipparchus Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter).
West side of Nansen Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter).

The area around craters may be rich in minerals. On Mars, heat from the impact melts ice in the ground. Water from the melting ice dissolves minerals, and then deposits them in cracks or faults that were produced with the impact. This process, called hydrothermal alteration, is a major way in which ore deposits are produced. The area around Martian craters may be rich in useful ores for the future colonization of Mars.[61] Studies on the earth have documented that cracks are produced and that secondary minerals veins are deposited in the cracks.[62][63][64] Images from satellites orbiting Mars have detected cracks near impact craters.[65] Great amounts of heat are produced during impacts. The area around a large impact may take hundreds of thousands of years to cool.[66][67][68] Many craters once contained lakes.[69][70][71] Because some crater floors show deltas, we know that water had to be present for some time. Dozens of deltas have been spotted on Mars.[72] Deltas form when sediment is washed in from a stream entering a quiet body of water. It takes a bit of time to form a delta, so the presence of a delta is exciting; it means water was there for a time, maybe for many years. Primitive organisms may have developed in such lakes; hence, some craters may be prime targets for the search for evidence of life on the Red Planet.[73]

List of cratersEdit

The following is a list of craters in the quadrangle. The crater's central location is of the quadrangle, craters that its central location is in another quadrangle is listed by eastern, western, northern or southern part.

Name Location Diameter Year of approval
Avire 40°49′S 159°46′W﻿ / ﻿40.82°S 159.76°W﻿ / -40.82; -159.76 6.85 km 2008
Copernicus 48°48′S 168°48′W﻿ / ﻿48.8°S 168.8°W﻿ / -48.8; -168.8 300 km 1973
Cross1 Southern part
Dechu 42°15′S 157°59′W﻿ / ﻿42.25°S 157.99°W﻿ / -42.25; -157.99 22 km 2018
Eudoxus 44°54′S 147°30′W﻿ / ﻿44.9°S 147.5°W﻿ / -44.9; -147.5 98 km 1973
Keeler 61°00′S 151°18′W﻿ / ﻿61°S 151.3°W﻿ / -61; -151.3 95 km 1973
Koval'sky1 Southern part 297 km1 1973
Kuiper 57°24′S 157°18′W﻿ / ﻿57.4°S 157.3°W﻿ / -57.4; -157.3 87 km 1973
Li Fan 47°12′S 153°12′W﻿ / ﻿47.2°S 153.2°W﻿ / -47.2; -153.2 104.8 km 1973
Liu Hsin 53°36′S 171°36′W﻿ / ﻿53.6°S 171.6°W﻿ / -53.6; -171.6 137 km 1973
Magelhaens 32°22′S 194°41′W﻿ / ﻿32.36°S 194.68°W﻿ / -32.36; -194.68 105 km
Mariner 35°06′S 164°30′W﻿ / ﻿35.1°S 164.5°W﻿ / -35.1; -164.5 170 km 1967
Nansen 50°18′S 140°36′W﻿ / ﻿50.3°S 140.6°W﻿ / -50.3; -140.6 81 km 1967
Newton 40°48′S 158°06′W﻿ / ﻿40.8°S 158.1°W﻿ / -40.8; -158.1 298 km 1973
Palikir 41°34′S 158°52′W﻿ / ﻿41.57°S 158.86°W﻿ / -41.57; -158.86 15.57 km 2011
Pickering 1973
Ptolemaeus 48°13′S 157°36′W﻿ / ﻿48.21°S 157.6°W﻿ / -48.21; -157.6 165 km 1973
Tyutaram 2013
Very 49°36′S 177°06′W﻿ / ﻿49.6°S 177.1°W﻿ / -49.6; -177.1 114.8 km 1973
Wright 58°54′S 151°00′W﻿ / ﻿58.9°S 151°W﻿ / -58.9; -151 113.7 km 1973

1Partly located in the quadrangle while another part is in a different quadrangle along with the crater's diameter

Linear ridge networksEdit

Linear ridge networks are found in various places on Mars in and around craters.[74] Ridges often appear as mostly straight segments that intersect in a lattice-like manner. They are hundreds of meters long, tens of meters high, and several meters wide. It is thought that impacts created fractures in the surface, these fractures later acted as channels for fluids. Fluids cemented the structures. With the passage of time, surrounding material was eroded away, thereby leaving hard ridges behind. Since the ridges occur in locations with clay, these formations could serve as a marker for clay which requires water for its formation.[75][76][77] Water here could have supported past life in these locations. Clay may also preserve fossils or other traces of past life.


Sand dunes have been found in many places on Mars. The presence of dunes shows that the planet has an atmosphere with wind, for dunes require wind to pile up the sand. Most dunes on Mars are black because of the weathering of the volcanic rock basalt.[78][79] Black sand can be found on Earth on Hawaii and on some tropical South Pacific islands.[80] Sand is common on Mars due to the old age of the surface that has allowed rocks to erode into sand. Dunes on Mars have been observed to move many meters.[81][82] Some dunes move along. In this process, sand moves up the windward side and then falls down the leeward side of the dune, thus caused the dune to go toward the leeward side (or slip face).[83] When images are enlarged, some dunes on Mars display ripples on their surfaces.[84] These are caused by sand grains rolling and bouncing up the windward surface of a dune. The bouncing grains tend to land on the windward side of each ripple. The grains do not bounce very high so it does not take much to stop them.


Much of the Martian surface is covered with a thick ice-rich, mantle layer that has fallen from the sky a number of times in the past.[85][86][87] In some places a number of layers are visible in the mantle.[88]


There is enormous evidence that water once flowed in river valleys on Mars.[89][90] Images of curved channels have been seen in images from Mars spacecraft dating back to the early seventies with the Mariner 9 orbiter.[91][92][93][94] Indeed, a study published in June 2017, calculated that the volume of water needed to carve all the channels on Mars was even larger than the proposed ocean that the planet may have had. Water was probably recycled many times from the ocean to rainfall around Mars.[95][96]

Dust devil tracksEdit

Because a thin coating of fine bright dust covers much of the surface of Mars, passing dust devils remove the bright dust and expose the underlying dark surface.[97][98] Dust devils have been seen from the ground and from orbiting spacecraft. They have even blown the dust off of the solar panels of the two Rovers on Mars, thereby greatly extending their lives.[99]

Other scenes in Phaethontis quadrangleEdit

Other Mars quadranglesEdit

Interactive Mars mapEdit


See alsoEdit


  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. (eds.). Mars. Tucson: University of Arizona Press. ISBN 978-0-8165-1257-7.
  2. ^ Blunck, J. 1982. Mars and its Satellites, Exposition Press. Smithtown, N.Y.
  3. ^ Murchie, S.; Mustard, John F.; Ehlmann, Bethany L.; Milliken, Ralph E.; et al. (2009). "A synthesis of Martian aqueous mineralogy after 1 Mars year of observations from the Mars Reconnaissance Orbiter" (PDF). Journal of Geophysical Research. 114: E00D06. Bibcode:2009JGRE..11400D06M. doi:10.1029/2009JE003342.
  4. ^ Grant, J.; Wilson, Sharon A.; Noe Dobrea, Eldar; Fergason, Robin L.; et al. (2010). "HiRISE views enigmatic deposits in the Sirenum Fossae region of Mars". Icarus. 205: 53–63. Bibcode:2010Icar..205...53G. doi:10.1016/j.icarus.2009.04.009.
  5. ^ Kieffer, Hugh H. (1992). Mars. Tucson: University of Arizona Press. pp. &#91, page&nbsp, needed&#93, . ISBN 978-0-8165-1257-7.
  6. ^
  7. ^ Irwin, Rossman P.; Howard, Alan D.; Maxwell, Ted A. (2004). "Geomorphology of Ma'adim Vallis, Mars, and associated paleolake basins". Journal of Geophysical Research. 109: 12009. Bibcode:2004JGRE..10912009I. doi:10.1029/2004JE002287.
  8. ^ Michael Carr (2006). The surface of Mars. Cambridge, UK: Cambridge University Press. pp. &#91, page&nbsp, needed&#93, . ISBN 978-0-521-87201-0.
  9. ^ Hartmann, W. (2003). A Traveler's Guide to Mars. New York: Workman Publishing. p. [page needed]. ISBN 978-0-7611-2606-5.
  10. ^
  11. ^
  12. ^
  14. ^ Edgett, K.; Malin, M. C.; Williams, R. M. E.; Davis, S. D. (2003). "Polar-and middle-latitude martian gullies: A view from MGS MOC after 2 Mars years in the mapping orbit" (PDF). Lunar Planet. Sci. 34. p. 1038, Abstract 1038. Bibcode:2003LPI....34.1038E.
  15. ^ a b Dickson, J; Head, J; Kreslavsky, M (2007). "Martian gullies in the southern mid-latitudes of Mars: Evidence for climate-controlled formation of young fluvial features based upon local and global topography" (PDF). Icarus. 188 (2): 315–323. Bibcode:2007Icar..188..315D. doi:10.1016/j.icarus.2006.11.020.
  16. ^
  17. ^ a b Heldmann, J; Mellon, Michael T (2004). "Observations of martian gullies and constraints on potential formation mechanisms" (PDF). Icarus. 168 (2): 285–304. Bibcode:2004Icar..168..285H. doi:10.1016/j.icarus.2003.11.024.
  19. ^
  21. ^ Malin, Michael C.; Edgett, Kenneth S. (2001). "Mars Global Surveyor Mars Orbiter Camera: Interplanetary cruise through primary mission". Journal of Geophysical Research. 106: 23429–23570. Bibcode:2001JGR...10623429M. doi:10.1029/2000JE001455.
  22. ^ Mustard, JF; Cooper, CD; Rifkin, MK (2001). "Evidence for recent climate change on Mars from the identification of youthful near-surface ground ice" (PDF). Nature. 412 (6845): 411–4. doi:10.1038/35086515. PMID 11473309.
  23. ^ Carr, Michael H. (2001). "Mars Global Surveyor observations of Martian fretted terrain". Journal of Geophysical Research. 106: 23571–23595. Bibcode:2001JGR...10623571C. doi:10.1029/2000JE001316.
  24. ^
  25. ^ Head, J. W.; Marchant, D. R.; Kreslavsky, M. A. (2008). "From the Cover: Formation of gullies on Mars: Link to recent climate history and insolation microenvironments implicate surface water flow origin". Proceedings of the National Academy of Sciences. 105 (36): 13258–63. Bibcode:2008PNAS..10513258H. doi:10.1073/pnas.0803760105. PMC 2734344. PMID 18725636.
  26. ^ Christensen, PR (2003). "Formation of recent martian gullies through melting of extensive water-rich snow deposits". Nature. 422 (6927): 45–8. Bibcode:2003Natur.422...45C. doi:10.1038/nature01436. PMID 12594459.
  27. ^
  28. ^ Jakosky, Bruce M.; Carr, Michael H. (1985). "Possible precipitation of ice at low latitudes of Mars during periods of high obliquity". Nature. 315 (6020): 559–561. Bibcode:1985Natur.315..559J. doi:10.1038/315559a0.
  29. ^ Jakosky, Bruce M.; Henderson, Bradley G.; Mellon, Michael T. (1995). "Chaotic obliquity and the nature of the Martian climate". Journal of Geophysical Research. 100: 1579–1584. Bibcode:1995JGR...100.1579J. doi:10.1029/94JE02801.
  30. ^ MLA NASA/Jet Propulsion Laboratory (December 18, 2003). "Mars May Be Emerging From An Ice Age". ScienceDaily. Retrieved February 19, 2009.
  31. ^ Hecht, M (2002). "Metastability of liquid water on Mars" (PDF). Icarus. 156 (2): 373–386. Bibcode:2002Icar..156..373H. doi:10.1006/icar.2001.6794.[permanent dead link]
  32. ^ Peulvast, J.P. (1988). "Mouvements verticaux et genèse du bourrelet Est-groenlandais. dans la région de Scoresby Sund". Physio Géo (in French). 18: 87–105.
  33. ^ Costard, F.; Forget, F.; Mangold, N.; Mercier, D.; et al. (2001). "Debris Flows on Mars: Analogy with Terrestrial Periglacial Environment and Climatic Implications" (PDF). Lunar and Planetary Science. XXXII: 1534. Bibcode:2001LPI....32.1534C.
  34. ^[permanent dead link],
  36. ^ a b c jawin, E, J. Head, D. Marchant. 2018. Transient post-glacial processes on Mars: Geomorphologic evidence for a paraglacial period. Icarus: 309, 187-206
  37. ^
  38. ^ Levy, J. et al. 2009. Concentric crater fill in Utopia Planitia: History and interaction between glacial "brain terrain" and periglacial processes. Icarus: 202. 462-476.
  39. ^ Levy, J.; Head, J.; Marchant, D. (2010). "Concentric Crater fill in the northern mid-latitudes of Mars: Formation process and relationships to similar landforms of glacial origin". Icarus. 209 (2): 390–404. Bibcode:2010Icar..209..390L. doi:10.1016/j.icarus.2010.03.036.
  40. ^ Levy, J.; Head, J.; Dickson, J.; Fassett, C.; Morgan, G.; Schon, S. (2010). "Identification of gully debris flow deposits in Protonilus Mensae, Mars: Characterization of a water-bearing, energetic gully-forming process". Earth Planet. Sci. Lett. 294 (3–4): 368–377. Bibcode:2010E&PSL.294..368L. doi:10.1016/j.epsl.2009.08.002.
  41. ^
  42. ^ Garvin, J., S. Sakimoto, J. Frawley. 2003. Craters on Mars: Geometric properties from gridded MOLA topography. In: Sixth International Conference on Mars. July 20–25, 2003, Pasadena, California. Abstract 3277.
  43. ^ Garvin, J. et al. 2002. Global geometric properties of martian impact craters. Lunar Planet. Sci: 33. Abstract # 1255.
  44. ^
  45. ^ Kreslavsky, M. and J. Head. 2006. Modification of impact craters in the northern planes of Mars: Implications for the Amazonian climate history. Meteorit. Planet. Sci.: 41. 1633-1646
  46. ^ Madeleine, J. et al. 2007. Exploring the northern mid-latitude glaciation with a general circulation model. In: Seventh International Conference on Mars. Abstract 3096.
  47. ^
  48. ^ Fastook, J., J.Head. 2014. Concentric crater fill: Rates of glacial accumulation, infilling and deglaciation in the Amazonian and Noachian of Mars. 45th Lunar and Planetary Science Conference (2014) 1227.pdf
  50. ^ Philippe Lognonné; François Forget; François Costard (2007). Planet Mars: Story of Another World (Springer Praxis Books / Popular Astronomy). Praxis. pp. &#91, page&nbsp, needed&#93, . ISBN 978-0-387-48925-4.
  51. ^ Fredric W. Taylor (2010). The Scientific Exploration of Mars. Cambridge, UK: Cambridge University Press. pp. &#91, page&nbsp, needed&#93, . ISBN 978-0-521-82956-4.
  52. ^ Connerney JE; Acuna MH; Wasilewski PJ; Reme; et al. (April 1999). "Magnetic lineations in the ancient crust of mars" (PDF). Science. 284 (5415): 794–8. Bibcode:1999Sci...284..794C. doi:10.1126/science.284.5415.794. PMID 10221909.
  53. ^ Langlais, B. (2004). "Crustal magnetic field of Mars" (PDF). Journal of Geophysical Research. 109: n/a. Bibcode:2004JGRE..10902008L. doi:10.1029/2003JE002048.[permanent dead link]
  54. ^ Connerney, J. E. P.; Acuña, MH; Ness, NF; Kletetschka, G; et al. (2005). "Tectonic implications of Mars crustal magnetism". Proceedings of the National Academy of Sciences. 102 (42): 14970–14975. Bibcode:2005PNAS..10214970C. doi:10.1073/pnas.0507469102. PMC 1250232. PMID 16217034.
  55. ^ Acuna, MH; Connerney, JE; Ness, NF; Lin, RP; Mitchell, D; Carlson, CW; McFadden, J; Anderson, KA; et al. (1999). "Global distribution of crustal magnetization discovered by the Mars Global Surveyor MAG/ER Experiment". Science. 284 (5415): 790–793. Bibcode:1999Sci...284..790A. doi:10.1126/science.284.5415.790. PMID 10221908.
  56. ^
  57. ^ Osterloo, M. M.; Hamilton, V. E.; Bandfield, J. L.; Glotch, T. D.; et al. (2008). "Chloride-Bearing Materials in the Southern Highlands of Mars". Science. 319 (5870): 1651–1654. Bibcode:2008Sci...319.1651O. CiteSeerX doi:10.1126/science.1150690. PMID 18356522.
  58. ^ Davila, A.; et al. (2011). "A large sedimentary basin in the Terra Sirenum region of the southern highlands of Mars". Icarus. 212 (2): 579–589. Bibcode:2011Icar..212..579D. doi:10.1016/j.icarus.2010.12.023.
  60. ^
  61. ^
  63. ^
  66. ^ name=""
  75. ^ Mangold; et al. (2007). "Mineralogy of the Nili Fossae region with OMEGA/Mars Express data: 2. Aqueous alteration of the crust". J. Geophys. Res. 112. Bibcode:2007JGRE..112.8S04M. doi:10.1029/2006JE002835.
  76. ^ Mustard et al., 2007. Mineralogy of the Nili Fossae region with OMEGA/Mars Express data: 1. Ancient impact melt in the Isidis Basin and implications for the transition from the Noachian to Hesperian, J. Geophys. Res., 112.
  77. ^ Mustard; et al. (2009). "Composition, Morphology, and Stratigraphy of Noachian Crust around the Isidis Basin". J. Geophys. Res. 114. Bibcode:2009JGRE..114.0D12M. doi:10.1029/2009JE003349.
  78. ^
  80. ^
  81. ^
  82. ^
  83. ^ Namowitz, S., Stone, D. 1975. earth science the world we live in. American Book Company. New York.
  84. ^
  85. ^ Hecht, M. 2002. Metastability of water on Mars. Icarus 156, 373–386
  86. ^ Mustard, J., et al. 2001. Evidence for recent climate change on Mars from the identification of youthful near-surface ground ice. Nature 412 (6845), 411–414.
  87. ^ Pollack, J., D. Colburn, F. Flaser, R. Kahn, C. Carson, and D. Pidek. 1979. Properties and effects of dust suspended in the martian atmosphere. J. Geophys. Res. 84, 2929-2945.
  88. ^
  95. ^
  97. ^
  98. ^
  99. ^
  101. ^ "Online Atlas of Mars". Retrieved December 16, 2012.

External linksEdit