Table of Contents Categories
  Encyclosphere.org ENCYCLOREADER
  supported by EncyclosphereKSF

Argyre quadrangle

Topic: Astronomy

 From HandWiki - Reading time: 19 min
Short description: Map of Mars
Argyre quadrangle
USGS-Mars-MC-26-ArgyreRegion-mola.png
Map of Argyre quadrangle from Mars Orbiter Laser Altimeter (MOLA) data. The highest elevations are red and the lowest are blue.
Coordinates [ ⚑ ] : 47°30′S 30°00′W / 47.5°S 30°W / -47.5; -30
Image of the Argyre Quadrangle (MC-26). The west-central part contains the Argyre basin, defined by a rim of rugged mountain blocks that surrounds a nearly circular expanse of light-colored plains. The large basin is surrounded by heavily cratered highlands.

The Argyre quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS) Astrogeology Research Program. The Argyre quadrangle is also referred to as MC-26 (Mars Chart-26).[1] It contains Argyre Planitia and part of Noachis Terra.

Name

The word Argyre is named after a legendary silver at the mouth of the Ganges--[Arakan, Berma.[2]

Main page: Astronomy:Classical albedo features on Mars

The Argyre quadrangle covers the area from 0° to 60° west longitude and from 30° to 65° south latitude on Mars. It contains Galle crater, which resembles a smiley face and the Argyre basin, a giant impact crater. Research published in the journal Icarus has found pits in Hale Crater that are caused by hot ejecta falling on ground containing ice. The pits are formed by heat forming steam that rushes out from groups of pits simultaneously, thereby blowing away from the pit ejecta.[3] Many steep slopes in this quadrangle contain gullies, which are believed to have formed by relatively recent flows of water.

Martian gullies

Gullies are common in some latitude bands on Mars. Usually, martian gullies are found on the walls of craters or troughs, but Charitum Montes, a group of mountains, has gullies in some areas (See the image below).

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,[4] others have found that the greater number of gullies are found on poleward facing slopes, especially from 30 to 44 S.[5][6]

Although many ideas have been put forward to explain them,[7] 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.[8][9] 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.

There is evidence for all three theories. Most of the gully alcove heads occur at the same level, just as one would expect of an aquifer. Various measurements and calculations show that liquid water could exist in aquifers at the usual depths where gullies begin.[8] One variation of this model is that rising hot magma could have melted ice in the ground and caused water to flow in aquifers. Aquifers are layer that allow water to flow. They may consist of porous sandstone. The aquifer layer would be perched on top of another layer that prevents water from going down (in geological terms it would be called impermeable). Because water in an aquifer is prevented from going down, the only direction the trapped water can flow is horizontally. Eventually, water could flow out onto the surface when the aquifer reaches a break—like a crater wall. The resulting flow of water could erode the wall to create gullies.[10] Aquifers are quite common on Earth. A good example is "Weeping Rock" in Zion National Park Utah.[11]

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.[12][13][14] This ice-rich mantle, a few yards thick, smooths 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.[15][16][17] 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.[18] The ice-rich mantle may be the result of climate changes.[19] 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.[20][21] When ice at the top of the mantling layer goes back into the atmosphere, it leaves behind dust, which insulating the remaining ice.[22] 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.[5][6] Higher elevations have far fewer gullies because ice would tend to sublimate more in the thin air of the higher altitude.[23]

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.[24] 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.[25][26] 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.[27]

  • Gullies on the western rim of Argyra Planitia as seen with CTX.

  • Charitum Montes Gullies, as seen by HiRISE

  • Gullies in Green Crater, as seen by HiRISE.

  • Close-up of gullies in Green Crater, as seen by HiRISE.

  • Jezza Crater, as seen by HiRISE. North wall (at top) has gullies. Dark lines are dust devil tracks. Scale bar is 500 meters long.

  • Gullies, as seen by HiRISE under HiWish program. Location is Nereidum Montes.

  • Scene in Argyre quadrangle with gullies, alluvival fans, and hollows, as seen by HiRISE under HiWish program. Enlargements of parts of this image are below.

  • Several levels of alluvial fans, as seen by HiRISE under HiWish program. Locations of these fans are indicated in the previous image.

  • Small, well-formed alluvial fan, as seen by HiRISE under HiWish program. Location of this fan is shown in an image displayed above.

  • Enlargement of above image showing hollows with box showing the size of a football field, as seen by HiRISE under HiWish program.

  • Gullies as seen by HiRISE under HiWish program.

  • Gullies in Nereidum Montes, as seen by HiRISE under HiWish program.

  • Gullies in a crater, as seen by HiRISE under HiWish program

  • Close up of gully aprons, as seen by HiRISE under HiWish program Note this is an enlargement of the previous image of gullies in a crater.

  • Wide view of gullies in Arkhangelsky Crater, as seen by HiRISE under HiWish program

  • Close-up of small channels in gullies in Arkhangelsky Crater, as seen by HiRISE under HiWish program Patterned ground in the shape of polygons can be seen to the right. Note: this is an enlargement of the previous image from Arkhangelsky Crater.

  • Close-up of a gully showing a channel going across the apron, as seen by HiRISE under HiWish program. Note: this is an enlargement of a previous image from Arkhangelsky Crater.

  • Gullies in crater, as seen by HiRISE under HiWish program

  • Close view of gullies from previous image The channels are quite curved. Because channels of gullies often form curves, it was thought that they were made by flowing water. Today, it is thought that they could be produced with chunks of dry ice. The image is from HiRISE under HiWish program.

  • Gullies on two sides of a mound, as seen by HiRISE under HiWish program

  • Gullies, as seen by HiRISE under HiWish program

  • Close view of gully channel, as seen by HiRISE under HiWish program Arrow shows small channel within larger channel. Small channel is quite curved in this image.

Argyre basin

The Argyre basin was created by a giant impact that occurred 70 million years after the Hellas impact.[28] It is believed to have contained a lake early in the history of Mars.[29] At least three river valleys (Surius Vallis, Dzigal Vallis, and Palacopus Vallis) drain into it from the south. After it froze solid, the ice formed eskers which are visible today.[30][31] An article written by 22 researchers in Icarus concluded that the impact that formed the Argyre basin probably stuck an ice cap or a thick permafrost layer. Energy from the impact melted the ice and formed a giant lake that eventually sent water to the North. The lakes's volume was equal to that of Earth's Mediterranean Sea. The deepest part of the lake may have taken more than a hundred thousand years to freeze, but with the help of heat from the impact, geothermal heating, and dissolved solutes it may have had liquid water for many millions of years. Life may have developed in this time. This region shows a great deal of evidence of glacial activity with flow features, crevasse-like fractures, drumlins, eskers, tarns, aretes, cirques, horns, U-shaped valleys, and terraces. Because of the shapes of Argyre sinuous ridges, the authors concluded that they are eskers.[32] Studies with advanced cameras, such as CTX, and MRO High Resolution Imaging Science Experiment (HiRISE) suggests that these ridges are probably eskers.[33][34]

  • Topography of the Argyre basin, the major feature in the Argyre quadrangle.

Galle (Martian crater)

  • Galle Crater, also called Happy-Face Crater, as seen by Mars Global Surveyor

  • Part of Galle Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter). The right eye and mouth are labeled. One of two dune fields are labeled as well.

  • Wide view of area around Galle Crater Colors show elevations.

  • Region around Galle Crater Colors show elevations.

  • Galle Crater Colors show elevations. Arrow indicates a layered mound that is enlarged in other images to follow.

  • Wide CTX view of part of layered mound. Parts of this mound are enlarged in HiRISE images that follow.

  • HiRISE image from area in previous image Picture taken under HiWish program.

  • Layers in mound in Galle Crater, as seen by HiRISE under HiWish program

  • Layers in mound in Galle Crater, as seen by HiRISE under HiWish program

  • Layers in mound in Galle Crater, as seen by HiRISE under HiWish program

  • Layers breaking up into boulders in Galle Crater, as seen by HiRISE under HiWish program

  • Layers and gullies in Galle Crater, as seen by HiRISE under HiWish program

  • Close view of layers in mound in Galle Crater, as seen by HiRISE under HiWish program

  • Layered mesa in mound in Galle Crater, as seen by HiRISE under HiWish program

  • Layers and polygons in mound in Galle Crater, as seen by HiRISE under HiWish program

  • Close view of layers in mound in Galle Crater, as seen by HiRISE under HiWish program

  • Unconformities in layers in Galle Crater, as seen by HiRISE Arrows point to some of the unconformities

Other craters

The older a surface is the more craters it will have; therefore the crater density of an area is used to determine the relative age.[35] Impact craters generally have a rim with ejecta around them, in contrast volcanic craters usually do not have a rim or ejecta deposits. As craters get larger (greater than 10 km in diameter) they usually have a central peak.[36] The peak is caused by a rebound of the crater floor following the impact.[37] Often, craters with diameters greater than 100 km have rings on their floors. Since so much material is blasted away, the ground readjusts, making circular faults. When lava flows upward along the faults, rings are produced.[38]

  • Wirtz Crater Dunes with ripples and frost, as seen by HiRISE.

  • Bond Crater Floor, as seen by HiRISE.

  • Hartwig Crater Floor, as seen by HiRISE. The scale bar is 500 meters long.

  • Baltisk Crater Floor, as seen by HiRISE. Scale bar is 1000 meters long. Dark dunes are visible at the bottom of image on the left.

  • Lohse Crater Gullies on Central Peak, as seen by HiRISE.

  • Arkhangelsky Crater Dunes, as seen by THEMIS. Click on image to see possible gullies on central peak.

  • East side of Halley Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter).

  • Floor of Halley Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter). Thin dark lines are dust devil tracks. Note: this is an enlargement of the previous image of Halley Crater.

  • West side of Vogel Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter).

  • Hooke Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter). Dark places are dunes.

  • Dust devil tracks in and around Hooke Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter). Note: this is an enlargement of the previous image of Hooke Crater.

  • Dunes and gullies in Hooke Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter). Note: this is an enlargement of a previous image of Hooke Crater.

  • Dunes and dust devil tracks in Hooke Crater, as seen by HiRISE. There are also gullies just visible.

  • Fan, layers, and dunes on the floor of Jones Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter). Note: this is an enlargement of the previous image of Jones Crater.

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

  • Dust devil tracks just outside rim of Maraldi Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter). Note: this is an enlargement of the previous image of Maraldi Crater.

  • East side of Helmholtz Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter).

  • Dunes and dust devil tracks in Helmholtz Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter). Note: this is an enlargement of the previous image of Helmholtz Crater.

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

  • Wegener Crater showing dunes defrosting, as seen by CTX camera (on Mars Reconnaissance Orbiter). Dark spots are places where frost has disappeared from the dark dunes. Note: this is an enlargement of the previous image of Wegener Crater.

  • Von Karman Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter). Dark parts near the top are dunes.

  • Defrosting dunes in Von Karman Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter). Dark places are where frost has left dark dunes. Picture taken in the springtime on Mars.

Layers

Layers may be formed by groundwater rising up depositing minerals and cementing sediments. The hardened layers are consequently more protected from erosion. This process may occur instead of layers forming under lakes. Some locations on the Red Planet show groups of layered rocks.[39][40] In some places the layers are arranged into regular patterns.[41][42] It has been suggested that the layers were put into place by volcanoes, the wind, or by being at the bottom of a lake or sea. Calculations and simulations show that groundwater carrying dissolved minerals would surface in the same locations that have abundant rock layers. According to these ideas, deep canyons and large craters would receive water coming from the ground. Many craters in the Arabia area of Mars contain groups of layers. Some of these layers may have resulted from climate change.

The tilt of the rotational axis of Mars has repeatedly changed in the past. Some changes are large. Because of these variations of climate, at times the atmosphere of Mars would have been much thicker and contained more moisture. The amount of atmospheric dust also has increased and decreased. It is believed that these frequent changes helped to deposit material in craters and other low places. The rising of mineral-rich ground water cemented these materials. The model also predicts that after a crater is full of layered rocks, additional layers will be laid down in the area around the crater. So, the model predicts that layers may also have formed in intercrater regions; layers in these regions have been observed.

Layers can be hardened by the action of groundwater. Martian ground water probably moved hundreds of kilometers, and in the process it dissolved many minerals from the rock it passed through. When ground water surfaces in low areas containing sediments, water evaporates in the thin atmosphere and leaves behind minerals as deposits and/or cementing agents. Consequently, layers of dust could not later easily erode away since they were cemented together. On Earth, mineral-rich waters often evaporate forming large deposits of various types of salts and other minerals. Sometimes water flows through Earth's aquifers, and then evaporates at the surface just as is hypothesized for Mars. One location this occurs on Earth is the Great Artesian Basin of Australia .[43] On Earth the hardness of many sedimentary rocks, like sandstone, is largely due to the cement that was put in place as water passed through.

  • Layers exposed in Nereidum Montes, as seen by HiRISE under HiWish program The light-toned layers may contain sulfates which are good for preserving traces of ancient life.

  • Close-up of layers from previous image, as seen by HiRISE under HiWish program

  • Low, layered mesa, as seen by HiRISE under HiWish program Arrows point to some layers.

  • Layers, as seen by HiRISE under HiWish program

  • Wide view of crater showing layers along wall, as seen by HiRISE under HiWish program

  • Close view of layers in crater wall, as seen by HiRISE under HiWish program

  • Layers in mesa on floor of crater, as seen by HiRISE under HiWish program

Channels

There is enormous evidence that water once flowed in river valleys on Mars.[44][45] Images of curved channels have been seen in images from Mars spacecraft dating back to the early seventies with the Mariner 9 orbiter.[46][47][48][49] 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.[50][51] Many places on Mars show channels of different sizes. Many of these channels probably carried water, at least for a time. The climate of Mars may have been such in the past that water ran on its surface. It has been known for some time that Mars undergoes many large changes in its tilt or obliquity because its two small moons lack the gravity to stabilize it, as the Moon stabilizes Earth; at times the tilt of Mars has even been greater than 80 degrees[52][53]

Main page: Astronomy:Outflow channels

  • Channel, as seen by HiRISE under HiWish program

  • Channel, as seen by HiRISE under HiWish program

  • Channels in Argyre quadrangle as seen by HiRISE, under the HiWish program. This is the image of the surface from a single HiRISE image. The scale bar at the top is 500 meters long.

  • Channel, as seen by HiRISE under HiWish program

Dust devil tracks

Dust devil tracks can be very pretty. They are caused by giant dust devils removing bright colored dust from the Martian surface; thereby exposing a dark layer. Dust devils on Mars have been photographed both from the ground and high overhead from orbit. They have even blown dust off the solar panels of two Rovers on Mars, thereby greatly extending their useful lifetime.[54] The pattern of the tracks has been shown to change every few months.[55] A study that combined data from the High Resolution Stereo Camera (HRSC) and the Mars Orbiter Camera (MOC) found that some large dust devils on Mars have a diameter of 700 metres (2,300 ft) and last at least 26 minutes.[56]

Main page: Astronomy:Dust devil tracks

  • Dust devil tracks and layers, as seen by HiRISE under HiWish program

  • Close, color view of dust devil tracks, as seen by HiRISE under HiWish program

  • Dust devil tracks as seen by HiRISE under HiWish program

  • Dust devil tracks, as seen by HiRISE under HiWish program

Dunes

  • Wide view of small dune field, as seen by HiRISE under HiWish program

  • Close view of dunes, as seen by HiRISE under HiWish program Ripples are visible on the dunes.

  • Field of dunes as seen by HiRISE

  • Close view of group of dunes, as seen by HiRISE under HiWish program

  • Single dune

Other features in Argyre quadrangle

  • Map of Argyre quadrangle with major features labeled. Galle crater looks like a smile.

  • CTX image showing context for the next image. A group of channels are visible in this image.

  • Close-up of surface in Argyre quadrangle, as seen by HiRISE, under the HiWish program.

  • Hollows, as seen by HiRISE under HiWish program

  • Possible pingos, as seen by HiRISE under HiWish program Pingos contain a core of ice. They are expected to have cracks on their surfaces because water expands when it turns into ice.

  • Wide view of polygons with ice in troughs between polygons, as seen by HiRISE under HiWish program

  • Close view of polygons with ice in troughs between polygons, as seen by HiRISE under HiWish program

  • Close view of polygons with ice in troughs between polygons, 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.[57][58] Quadrangle numbers (beginning with MC for "Mars Chart")[59] 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

Error: Image is invalid or non-existent.


See also


References

  1. ↑ Davies, M.E.; Batson, R.M.; Wu, S.S.C. "Geodesy and Cartography" in Kieffer, H.H.; Jakosky, B.M.; Snyder, C.W.; Matthews, M.S., Eds. Mars. University of Arizona Press: Tucson, 1992.
  2. ↑ Blunck, J. 1982. Mars and its Satellites. Exposition Press. Smithtown, N.Y.
  3. ↑ Tornabene, L. (2012). "Widespread crater-related pitted materials on Mars. Further evidence for the role of target volatiles during the impact process". Icarus 220 (2): 348–368. doi:10.1016/j.icarus.2012.05.022. Bibcode: 2012Icar..220..348T. 
  4. ↑ Edgett, K. et al. 2003. Polar-and middle-latitude martian gullies: A view from MGS MOC after 2 Mars years in the mapping orbit. Lunar Planet. Sci. 34. Abstract 1038.
  5. ↑ 5.0 5.1 "Archived copy". http://www.planetary.brown.edu/pdfs/3138.pdf. 
  6. ↑ 6.0 6.1 Dickson, J. (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". Icarus 188 (2): 315–323. doi:10.1016/j.icarus.2006.11.020. Bibcode: 2007Icar..188..315D. 
  7. ↑ "PSRD: Gullied Slopes on Mars". http://www.psrd.hawaii.edu/Aug03/MartianGullies.html. 
  8. ↑ 8.0 8.1 Heldmann, J.; Mellon, M. (2004). "Observations of martian gullies and constraints on potential formation mechanisms". Icarus 168 (2): 285–304. doi:10.1016/j.icarus.2003.11.024. Bibcode: 2004Icar..168..285H. https://zenodo.org/record/1259029. 
  9. ↑ Forget, F. et al. 2006. Planet Mars Story of Another World. Praxis Publishing. Chichester, UK.
  10. ↑ "Mars Gullies Likely Formed By Underground Aquifers". Space.com. 12 November 2004. http://www.space.com/scienceastronomy/mars_aquifer_041112.html. 
  11. ↑ Harris, A and E. Tuttle. 1990. Geology of National Parks. Kendall/Hunt Publishing Company. Dubuque, Iowa
  12. ↑ Malin, M.; Edgett, K. (2001). "Mars Global Surveyor Mars Orbiter Camera: Interplanetary cruise through primary mission". J. Geophys. Res. 106 (E10): 23429–23570. doi:10.1029/2000je001455. Bibcode: 2001JGR...10623429M. 
  13. ↑ Mustard, J. (2001). "Evidence for recent climate change on Mars from the identification of youthful near-surface ground ice". Nature 412 (6845): 411–414. doi:10.1038/35086515. PMID 11473309. Bibcode: 2001Natur.412..411M. 
  14. ↑ Carr, M (2001). "Mars Global Surveyor observations of fretted terrain". J. Geophys. Res. 106 (E10): 23571–23595. doi:10.1029/2000je001316. Bibcode: 2001JGR...10623571C. 
  15. ↑ "Martian gullies could be scientific gold mines". NBC News. http://www.nbcnews.com/id/15702457. 
  16. ↑ Head, JW; Marchant, DR; Kreslavsky, MA (September 2008). "Formation of gullies on Mars: Link to recent climate history and insolation microenvironments implicate surface water flow origin". Proc. Natl. Acad. Sci. U.S.A. 105 (36): 13258–63. doi:10.1073/pnas.0803760105. PMID 18725636. Bibcode: 2008PNAS..10513258H. 
  17. ↑ Head, J. (2008). "Formation of gullies on Mars: Link to recent climate history and insolation microenvironments implicate surface water flow origin". PNAS 105 (36): 13258–13263. doi:10.1073/pnas.0803760105. PMID 18725636. Bibcode: 2008PNAS..10513258H. 
  18. ↑ Christensen, P (2003). "Formation of recent martian gullies through melting of extensive water-rich snow deposits". Nature 422 (6927): 45–48. doi:10.1038/nature01436. PMID 12594459. Bibcode: 2003Natur.422...45C. 
  19. ↑ "Melting Snow Created Mars Gullies, Expert Says". http://news.nationalgeographic.com/news/2008/03/080319-mars-gullies_2.html. 
  20. ↑ Jakosky, B.; Carr, M. (1985). "Possible precipitation of ice at low latitudes of Mars during periods of high obliquity". Nature 315 (6020): 559–561. doi:10.1038/315559a0. Bibcode: 1985Natur.315..559J. https://zenodo.org/record/1233025. 
  21. ↑ Jakosky, B. (1995). "Chaotic obliquity and the nature of the Martian climate". J. Geophys. Res. 100 (E1): 1579–1584. doi:10.1029/94je02801. Bibcode: 1995JGR...100.1579J. 
  22. ↑ https://www.sciencedaily.com/releases/2003/12/031218075443.htmAds [yes|permanent dead link|dead link}}]
  23. ↑ Hecht, M (2002). "Metastability of liquid water on Mars". Icarus 156 (2): 373–386. doi:10.1006/icar.2001.6794. Bibcode: 2002Icar..156..373H. 
  24. ↑ Peulvast, J. Physio-Geo. 18. 87-105.
  25. ↑ Costard, F. et al. 2001. Debris Flows on Mars: Analogy with Terrestrial Periglacial Environment and Climatic Implications. Lunar and Planetary Science XXXII (2001). 1534.pdf
  26. ↑ http://www.spaceref.com:16090/news/viewpr.html?pid=7124 [yes|permanent dead link|dead link}}]
  27. ↑ Clow, G (1987). "Generation of liquid water on Mars through the melting of a dusty snowpack". Icarus 72 (1): 93–127. doi:10.1016/0019-1035(87)90123-0. Bibcode: 1987Icar...72...95C. 
  28. ↑ Robbins (2013). "large impact crater histories of Mars: The effect of different model crater age techniques". Icarus 225 (1): 173–184. doi:10.1016/j.icarus.2013.03.019. Bibcode: 2013Icar..225..173R. 
  29. ↑ Parker, T. et al. 2000. Argyre Planitia and the Mars global hydrolocia cycle. LPSC XXXI. Abstract 2033
  30. ↑ Kargel, J. and R. Strom. 1991. Terrestrial glacial eskers: analogs for martian sinuous ridges. LPSC XXII, 683-684.
  31. ↑ Michael H. Carr (2006). The surface of Mars. Cambridge University Press. ISBN 978-0-521-87201-0. https://books.google.com/books?id=uLHlJ6sjohwC. Retrieved 21 March 2011. 
  32. ↑ Dohm, J.; Hare, T.; Robbins, S.; Williams, J.-P.; Soare, R.; El-Maarry, M.; Conway, S.; Buczkowski, D. et al. (2015). "Geological and hydrological histories of the Argyre province, Mars". Icarus 253: 66–98. doi:10.1016/j.icarus.2015.02.017. Bibcode: 2015Icar..253...66D. https://hal-insu.archives-ouvertes.fr/insu-02274347/file/Dohm%20et%20al.%20Argyre_basin_MS_1_31_2015_track-changed_final%20version_finali....pdf. 
  33. ↑ Banks, M.; Lang, N.; Kargel, J.; McEwen, A.; Baker, V.; Grant, J.; Pelletier, J.; Strom, R. (2009). "An analysis of sinuous ridges in the southern Argyre Planitia, Mars using HiRISE and CTX images and MOLA data". J. Geophys. Res. 114 (E9): E09003. doi:10.1029/2008JE003244. Bibcode: 2009JGRE..114.9003B. 
  34. ↑ Bernhardt, H.; Hiesinger, H.; Reiss, D.; Ivanov, M.; Erkeling, G. (2013). "Putative eskers and new insights into glacio-fluvial depositional settings southern Argyre Planitia, Mars". Planet. Space Sci. 85: 261–278. doi:10.1016/j.pss.2013.06.022. Bibcode: 2013P&SS...85..261B. 
  35. ↑ "Shaping the Planets: Impact Cratering". http://www.lpi.usra.edu/education/explore/shaping_the_planets/impact-cratering/. 
  36. ↑ "Stones, Wind, and Ice: A Guide to Martian Impact Craters". http://www.lpi.usra.edu/publications/slidesets/stones/. 
  37. ↑ Hugh H. Kieffer (1992). Mars. University of Arizona Press. ISBN 978-0-8165-1257-7. https://books.google.com/books?id=NoDvAAAAMAAJ. Retrieved 7 March 2011. 
  38. ↑ Forget, F. et al. 2006. Planet Mars Story of Another World. Praxis Publishing. Chichester, UK
  39. ↑ Edgett, Kenneth S. (2005). "The sedimentary rocks of Sinus Meridiani: Five key observations from data acquired by the Mars Global Surveyor and Mars Odyssey orbiters". The Mars Journal 1: 5–58. doi:10.1555/mars.2005.0002. Bibcode: 2005IJMSE...1....5E. 
  40. ↑ Malin, M. P.; Edgett, K. S. (2000). "Ancient sedimentary rocks of early Mars". Science 290 (5498): 1927–1937. doi:10.1126/science.290.5498.1927. PMID 11110654. Bibcode: 2000Sci...290.1927M. 
  41. ↑ Lewis, K. W.; Aharonson, O.; Grotzinger, J. P.; Kirk, R. L.; McEwen, A. S.; Suer, T.-A. (2008). "Quasi-Periodic Bedding in the Sedimentary Rock Record of Mars". Science 322 (5907): 1532–5. doi:10.1126/science.1161870. PMID 19056983. Bibcode: 2008Sci...322.1532L. https://authors.library.caltech.edu/12528/2/LEWsci08supp.pdf. 
  42. ↑ Lewis, K. W., O. Aharonson, J. P. Grotzinger, A. S. McEwen, and R. L. Kirk (2010), Global significance of cyclic sedimentary deposits on Mars, Lunar Planet. Sci., XLI, Abstract 2648.
  43. ↑ Habermehl, M. A. (1980). "The Great Artesian Basin, Australia". J. Austr. Geol. Geophys. 5: 9–38. 
  44. ↑ Baker, V. (2015). "Fluvial geomorphology on Earth-like planetary surfaces: a review". Geomorphology 245: 149–182. doi:10.1016/j.geomorph.2015.05.002. PMID 29176917. 
  45. ↑ Carr, M. 1996. in Water on Mars. Oxford Univ. Press.
  46. ↑ Baker, V. 1982. The Channels of Mars. Univ. of Tex. Press, Austin, TX
  47. ↑ Baker, V.; Strom, R.; Gulick, V.; Kargel, J.; Komatsu, G.; Kale, V. (1991). "Ancient oceans, ice sheets and the hydrological cycle on Mars". Nature 352 (6336): 589–594. doi:10.1038/352589a0. Bibcode: 1991Natur.352..589B. 
  48. ↑ Carr, M (1979). "Formation of Martian flood features by release of water from confined aquifers". J. Geophys. Res. 84: 2995–300. doi:10.1029/jb084ib06p02995. Bibcode: 1979JGR....84.2995C. 
  49. ↑ Komar, P (1979). "Comparisons of the hydraulics of water flows in Martian outflow channels with flows of similar scale on Earth". Icarus 37 (1): 156–181. doi:10.1016/0019-1035(79)90123-4. Bibcode: 1979Icar...37..156K. 
  50. ↑ "How Much Water Was Needed to Carve Valleys on Mars? - SpaceRef". 5 June 2017. http://spaceref.com/mars/how-much-water-was-needed-to-carve-valleys-on-mars.html. 
  51. ↑ Luo, W. (2017). "New Martian valley network volume estimate consistent with ancient ocean and warm and wet climate". Nature Communications 8: 15766. doi:10.1038/ncomms15766. PMID 28580943. Bibcode: 2017NatCo...815766L. 
  52. ↑ name; Touma, J.; Wisdom, J. (1993). "The Chaotic Obliquity of Mars". Science 259 (5099): 1294–1297. doi:10.1126/science.259.5099.1294. PMID 17732249. Bibcode: 1993Sci...259.1294T. 
  53. ↑ Laskar, J.; Correia, A.; Gastineau, M.; Joutel, F.; Levrard, B.; Robutel, P. (2004). "Long term evolution and chaotic diffusion of the insolation quantities of Mars". Icarus 170 (2): 343–364. doi:10.1016/j.icarus.2004.04.005. Bibcode: 2004Icar..170..343L. 
  54. ↑ Mars Exploration Rover Mission: Press Release Images: Spirit. Marsrovers.jpl.nasa.gov. Retrieved on 7 August 2011.
  55. ↑ "HiRISE | Dust Devils Dancing on Dunes (PSP_005383_1255)". https://hirise.lpl.arizona.edu/PSP_005383_1255. 
  56. ↑ Reiss, D. (2011). "Multitemporal observations of identical active dust devils on Mars with High Resolution Stereo Camera (HRSC) and Mars Orbiter Camera (MOC)". Icarus 215 (1): 358–369. doi:10.1016/j.icarus.2011.06.011. Bibcode: 2011Icar..215..358R. 
  57. ↑ Morton, Oliver (2002). Mapping Mars: Science, Imagination, and the Birth of a World. New York: Picador USA. p. 98. ISBN 0-312-24551-3. 
  58. ↑ "Online Atlas of Mars". http://ralphaeschliman.com/id30.htm. Retrieved December 16, 2012. 
  59. ↑ "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



Retrieved from "https://handwiki.org/wiki/index.php?title=Astronomy:Argyre_quadrangle&oldid=3346993"
Licensed under CC BY-SA 3.0 | Source: https://handwiki.org/wiki/Astronomy:Argyre_quadrangle
21 views | Status: cached on August 18 2024 11:02:13
↧ Download this article as ZWI file
Encyclosphere.org EncycloReader is supported by the EncyclosphereKSF