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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. Water here could have supported past life in these locations. Clay may also preserve fossils or other traces of past life.
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its "strange cobweb-like networks of ridges and crags smoother areas into a pattern something like fragments of a broken plate." Both land masses' shapes have been formed by lava flows from volcanic eruptions, causing both surfaces to be covered by a thick layer of hardened lava. Findings from aerial footage of both
Amazonis and Iceland have shown nearly identical terrain patterns, signifying the comparative ages of the two regions.
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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 than the Earth's. That is, the difference between the farthest point from the Sun and the closest point to the Sun is very great
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is a soft, easily eroded deposit that extends for nearly 1,000 km along the equator of Mars. The surface of the formation has been eroded by the wind into a series of linear ridges called yardangs. These ridges generally point in direction of the prevailing winds that carved them and demonstrate
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Although the full implications of
Amazonis's youth have not yet been determined, the nature of the area (i.e. lack of sedimentary rock) has at least provided researchers evidence that the areas are the most likely to provide future discoveries, and as such, has been proposed as a future site for most
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because researchers originally (and incorrectly) thought
Amazonis Planitia to be representative of all Martian plains. Instead, over the past two decades, researchers have realized that the area's youth and extremely smooth surface actually distinguish the area from its neighbors. It is even possible
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Amazonis has become the primary focus of modern research efforts both because of its geological composition and because of its relative youth compared to other
Martian regions, which are often hundreds of millions of years older. Hartman writes that the plain closely resembles Iceland's surface, with
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are found in various places on Mars in and around craters. 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
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walls. It seems that the youngest streaks are dark and they become lighter with age. Often they begin as a small narrow spot then widen and extend downhill for hundreds of meters. Several ideas have been advanced to explain the streaks. Some involve
698:
It is most generally accepted that the streaks represent avalanches of dust. Streaks appear in areas covered with dust. When a thin layer of dust is removed, the underlying surface appears dark. Much of the
Martian surface is covered with dust.
686:. The streaks appear in areas covered with dust. Much of the Martian surface is covered with dust because at more or less regular intervals dust settles out of the atmosphere covering everything. We know a lot about this dust because the
764:
Brain terrain is common in many places on Mars. It is formed when ice sublimates along cracks. The ridges of brain terrain may contain a core of ice. Shadow measurements from HiRISE indicate the ridges are 4–5 meters high.
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get covered with dust. The power of the Rovers has been saved many times by the wind, in the form of dust devils that have cleared the panels and boosted the power. So we know that dust falls from the atmosphere frequently.
1246:
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.,
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Head, J., J. Mustard. 2006. Breccia dikes and crater-related faults in impact craters on Mars: Erosion and exposure on the floor of a crater 75 km in diameter at the dichotomy boundary, Meteorit. Planet
Science: 41,
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When a fluid moves by a feature like a mound, it will become streamlined. Often flowing water makes the shape and later lava flows spread over the region. In the pictures below this has occurred.
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Levy, J., J. Head, D. Marchant. 2009. Concentric crater fill in Utopia
Planitia: History and interaction between glacial “brain terrain” and periglacial mantle processes. Icarus 202, 462–476.
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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, doi:10.1029/2006JE002835.
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867:. The ridges were probably once stream valleys that have become full of sediment and cemented. So, they became hardened against erosion which removed surrounding material.
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Fuller, E.R. and J.W. Head III (2002), Amazonis
Planitia: The role of geologically recent volcanism and sedimentation in the formation of the smoothest plains on Mars.
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Mustard et al., 2009. Composition, Morphology, and Stratigraphy of Noachian Crust around the Isidis Basin, J. Geophys. Res., 114, doi:10.1029/2009JE003349.
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the erosive power of Martian winds. The easily eroded nature of the Medusae Fossae Formation suggests that it is composed of weakly cemented particles,
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over the image to see the names of over 60 prominent geographic features, and click to link to them. Coloring of the base map indicates relative
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craft arrived there, nothing could be seen through the dust storm. Other global dust storms have also been observed, since that time.
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for Mars, but only slight for the Earth. Also, every few years, the entire planet is engulfed in a global dust storm. When NASA's
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Hartmann, William. A Traveler's Guide to Mars: The Mysterious Landscapes of the Red Planet. Workman Publishing: New York, 2003.
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Lava flows affected by obstacles, as seen by HiRISE under HiWish program Arrows show two obstacles that are changing the flow.
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226:. The plain's topography exhibits extremely smooth features at several different lengths of scale. A large part of the
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Narrow ridges, as seen by HiRISE under HiWish program. The ridges may be the result of impacts fracturing the surface.
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Close view of a lava lobe, as seen by HiRISE under HiWish program The box shows the size of a football field.
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Close-up of ridge network, as seen by HiRISE under HiWish program This is an enlargement of a previous image.
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Close-up of ridge network, as seen by HiRISE under HiWish program This is an enlargement of a previous image.
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1162:"GEOLOGIC HISTORY OF THE SMOOTHEST PLAINS ON MARS (AMAZONIS PLANITIA) AND ASTROBIOLOGICAL IMPLICATIONS."
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View of a lava lobe, as seen by HiRISE under HiWish program The box shows the size of a football field.
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Close view of ridge network, as seen by HiRISE under HiWish program Box shows size of football field.
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MOLA map showing boundaries for Amazonis Planitia and other regions Colors indicate elevations.
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impeding viewing of the Martian terrain, and closely resemble the composition of Earth's
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Layers in Gordii Dorsum Region, as seen by HiRISE under HiWish program. Dark lines are
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Wide view of streamlined shape and rafts of lava, as seen by HiRISE under HiWish program
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Yardangs, as seen by HiRISE under HiWish program Location is near Gordii Dorsum in the
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that the area possessed distinctive characteristics when all of Mars was under water.
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Close view of lava rafts from previous images, as seen by HiRISE under HiWish program
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Closer view of previous image, showing layers, as seen by HiRISE under HiWish program
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Dark slope streaks on mound in Lycus Sulci, as seen by HiRISE under HiWish program
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Plateau made up of Medusae Fossae materials and rootless cones, as seen by HiRISE.
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Only approximately 100 million years old, these plains provide some of the fewest
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Close view of layers from previous image, as seen by HiRISE under HiWish program
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Grotzinger, J. and R. Milliken (eds.) 2012. Sedimentary Geology of Mars. SEPM
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Layers in trough and dark slope streaks, as seen by HiRISE under HiWish program
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Dark slope streaks on mesa, as seen by HiRISE under HiWish program Location is
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as a "bright dusty volcanic desert crossed by many fresh-looking lava flows."
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Close, color view of polygonal ridges, as seen by HiRISE under HiWish program
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Close, color view of brain terrain, as seen by HiRISE under HiWish program
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Wide view of scarp showing layers, as seen by HiRISE under HiWish program
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Streamlined shape showing layers, as seen by HiRISE under HiWish program.
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Wide view of large ridge network, as seen by HiRISE under HiWish program
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Surfaces in Amazonis quadrangle, as seen by HiRISE under HiWish program.
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Layered features in Lycus Sulci, as seen by HiRISE under HiWish program
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http://www.space.com/scienceastronomy/streaks_mars_streaks_030328.html
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Lunar and Planetary Science XXXIII (2002). URL accessed 19 April 2006.
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Close view of polygonal ridges, as seen by HiRISE under HiWish program
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Pedestal crater with layers, as seen by HiRISE under HiWish program
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Close view of brain terrain, as seen by HiRISE under HiWish program
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Close, color view of ridges, as seen by HiRISE under HiWish program
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Wide view of polygon ridges, as seen by HiRISE under HiWish program
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Wide view of brain terrain, as seen by HiRISE under HiWish program
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observed by early astronomers, which was in turn named after the
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1328:"Mars Spirit Rover Gets Energy Boost from Cleaner Solar Panels"
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http://www.space.com/scienceastronomy/streaks_mars_021200.html
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Linear ridge networks, as seen by HiRISE under HiWish program
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Linear ridge networks, as seen by HiRISE under HiWish program
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Polygonal ridges, as seen by HiRISE under HiWish program
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Polygonal ridges, as seen by HiRISE under HiWish program
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Polygonal ridges, as seen by HiRISE under HiWish program
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The entire contemporary era on Mars has been named the
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Google Mars zoomable map centered on Amazonis Planitia
590:, as seen by HiRISE. Click on image for good view of
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1051:. Whites and browns indicate the highest elevations (
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across great plains, Amazonis has been described by
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334:Yardangs near a crater, as seen by HiRISE under
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1417:HiRISE image of faulting in Amazonis Planitia
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1301:: CS1 maint: archived copy as title (
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859:Possible inverted stream channels in
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241:, a mythical race of warrior women.
171:) is one of the smoothest plains on
183:volcanic provinces, to the west of
13:
1160:E. R. Fuller and J. W. Head, III,
807:More Images from Amazonis Planitia
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594:. Island is just to the west of
233:Its name derives from one of the
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863:region, as seen by HiRISE under
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598:. Scale bar is 500 meters long.
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1372:. University of Arizona Press.
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1341:Moore, Patrick (2 June 1990).
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175:. It is located between the
1859:Recurring slope lineae (RSL)
1043:Mars Orbiter Laser Altimeter
671:dark streaks on steep slopes
7:
2293:Inspiration Mars Foundation
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230:lies in Amazonis Planitia.
10:
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2328:Artificial objects on Mars
2397:
2345:List of films set on Mars
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2160:C/2013 A1 (Siding Spring)
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1957:Classical albedo features
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1343:Atlas of the Solar System
1041:, based on data from the
1031:global topography of Mars
257:. Formed by free-flowing
235:classical albedo features
55:
24:
2263:List of missions to Mars
1451:
1366:Hugh H. Kieffer (1992).
1143:Medusae Fossae Formation
682:, or even the growth of
291:Medusae Fossae Formation
285:Medusae Fossae Formation
228:Medusae Fossae Formation
46:colorized relief map of
2421:Solar System portal
2035:Solar eclipses on Mars
1894:"Swiss cheese" feature
1750:Concentric crater fill
1138:List of plains on Mars
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586:Streamlined Island in
1027:Interactive image map
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353:Linear ridge networks
348:Linear ridge networks
2235:Permanent settlement
1048:Mars Global Surveyor
945:Interactive Mars map
193:Memnonia quadrangles
2474:Memnonia quadrangle
2469:Amazonis quadrangle
2377:Timekeeping on Mars
2054:Planetary transits
2039:Satellite transits
1952:Observation history
1800:Lobate debris apron
738:Amazonis quadrangle
340:Amazonis quadrangle
338:Location is in the
320:Amazonis quadrangle
245:Age and composition
210: /
73: /
31:Topographic map of
21:
1128:Dark slope streaks
1110:
839:(April 10, 2001) (
833:Martian Dust Devil
722:Dark Slope Streaks
660:Dark slope streaks
592:Dark Slope Streaks
534:Streamlined shapes
251:sedimentary layers
19:
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2382:Sol (day on Mars)
2350:Martian scientist
2333:Memorials on Mars
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2287:The Case for Mars
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1899:Terrain softening
1864:Ring mold craters
1832:North Polar Basin
1755:Dark slope streak
1600:Vastitas Borealis
1497:Dust devil tracks
1379:978-0-8165-1257-7
1133:Geography of Mars
1095:Mars Memorial map
1053:+12 to +8 km
837:Amazonis Planitia
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33:Amazonis Planitia
20:Amazonis Planitia
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281:NASA landings.
274:Amazonian Epoch
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105:
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81:
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62:
60:
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17:
12:
11:
5:
2487:
2477:
2476:
2471:
2466:
2464:Plains on Mars
2451:
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2427:
2426:
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2423:
2410:
2398:
2395:
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2298:Mars Institute
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2119:
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2102:
2085:
2079:
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2071:
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2060:
2052:
2051:
2050:
2045:
2037:
2031:
2029:
2023:
2022:
2020:
2019:
2018:
2017:
2012:
2002:
2001:
2000:
1995:
1984:
1982:
1973:
1967:
1966:
1963:
1962:
1960:
1959:
1954:
1949:
1944:
1939:
1933:
1931:
1925:
1924:
1922:
1921:
1916:
1911:
1906:
1901:
1896:
1891:
1886:
1881:
1876:
1874:Seasonal flows
1871:
1869:Rootless cones
1866:
1861:
1856:
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1844:
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1709:
1704:
1699:
1697:Valley network
1694:
1689:
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1682:Observed rocks
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1657:
1652:
1647:
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1597:
1595:Ultimi Scopuli
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1575:Terra Cimmeria
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1407:
1406:External links
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1308:
1269:
1258:
1249:
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1211:
1209:Hartmann, 287.
1202:
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1191:Hartmann, 286.
1184:
1182:Hartmann, 275.
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865:HiWish program
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336:HiWish program
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246:
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214:24.8°N 196.0°E
195:, centered at
90:
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2230:Human mission
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2225:Sample return
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2088:Mars-crossers
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1904:Tharsis bulge
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1736:
1735:Chaos terrain
1733:
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1725:Brain terrain
1723:
1722:
1720:
1718:
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1640:Chaos terrain
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1555:Planum Boreum
1553:
1551:
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1546:
1545:Olympia Undae
1543:
1541:
1538:
1536:
1535:Eridania Lake
1533:
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1352:0-517-00192-6
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1284:on 2015-02-21
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1082:
1081:Polar regions
1078:
1074:
1070:
1059:); yellow is
1050:
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930:
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906:
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861:Phlegra Dorsa
855:
850:
846:
845:video (02:19)
842:
838:
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828:
823:
816:
811:
810:
797:
792:
785:
780:
773:
768:
767:
766:
760:
759:Brain terrain
748:
743:
739:
732:
727:
723:
716:
711:
710:
709:
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702:
696:
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672:
668:
661:
649:
644:
637:
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619:
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601:
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596:Pettit Crater
593:
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164:
99:
98:
86:
58:
54:
49:
45:
42:
40:
34:
28:
23:
2448:Solar System
2367:Life on Mars
2362:Flag of Mars
2303:Mars Society
2285:
2278:
2245:Terraforming
2240:Colonization
2010:Swift crater
1852:polar wander
1580:Terra Sabaea
1520:Arabia Terra
1395:
1383:. Retrieved
1368:
1361:
1342:
1336:
1322:
1311:
1286:. Retrieved
1282:the original
1272:
1261:
1252:
1242:
1233:
1223:
1214:
1205:
1196:
1187:
1178:
1169:
1156:
1112:
1093:
1087:
1046:
836:
763:
697:
688:solar panels
664:
588:Marte Vallis
537:
351:
288:
279:
271:
267:
248:
232:
185:Olympus Mons
168:
94:
93:
47:
36:
32:
2190:Exploration
2112:5261 Eureka
1780:Groundwater
1745:Composition
1570:Tempe Terra
1560:Quadrangles
1487:Circulation
1086:(See also:
1083:are noted.
701:Dust storms
692:Mars rovers
219:24.8; 196.0
217: /
82:24.8; 196.0
80: /
56:Coordinates
2458:Categories
1847:Polar caps
1827:Mud cracks
1810:Meteorites
1795:Lava tubes
1730:Carbonates
1665:Labyrinthi
1540:Iani Chaos
1479:Atmosphere
1288:2010-12-19
1228:1675-1690.
1149:References
1065:−8 km
1045:on NASA's
1039:elevations
1035:your mouse
673:, such as
616:Lava flows
2372:Sub-Earth
2355:Mythology
2308:Mars race
2075:Asteroids
1971:Astronomy
1942:Hesperian
1937:Amazonian
1909:Volcanism
1884:Spherules
1805:Marsquake
1760:Dichotomy
1675:by height
1670:Mountains
1470:Geography
1077:longitude
1061:0 km
706:Mariner 9
684:organisms
187:, in the
95:Amazonis
2408:Category
2272:Advocacy
2255:Missions
2198:Concepts
2027:Transits
1998:Monolith
1947:Noachian
1919:Yardangs
1815:on Earth
1775:Glaciers
1620:"Canals"
1612:features
1610:Physical
1297:cite web
1117:See also
1073:latitude
1033:. Hover
205:196°00′E
189:Amazonis
169:Amāzŏnis
167:, Latin
97:Planitia
68:196°00′E
2340:Fiction
2321:Related
2215:Landing
2210:Orbiter
2169:General
2138:2007 NS
2128:1999 UJ
2118:1998 VF
2107:Trojans
2094:2007 WD
2083:Impacts
2063:Mercury
1929:History
1889:Surface
1820:on Mars
1785:Gullies
1770:Geysers
1717:Geology
1707:Gravity
1702:Valleys
1655:Gullies
1645:Craters
1635:Catenae
1630:Canyons
1585:Tharsis
1530:Cydonia
1512:Regions
1502:Methane
1492:Climate
1385:7 March
1104:discuss
1029:of the
255:Iceland
239:Amazons
202:24°48′N
181:Elysium
177:Tharsis
65:24°48′N
2434:Portal
2412:
2401:
2153:Comets
2048:Deimos
2043:Phobos
2005:Deimos
1988:Phobos
1692:Plains
1660:Mensae
1650:Fossae
1376:
1349:
675:crater
2220:Rover
2205:Flyby
2176:Orbit
2058:Earth
1980:Moons
1914:Water
1790:Lakes
1740:Color
1590:Undae
835:- in
680:water
669:show
1879:Soil
1624:list
1453:Mars
1387:2011
1374:ISBN
1369:Mars
1347:ISBN
1303:link
1247:112.
1100:view
1092:and
1075:and
1071:are
1069:Axes
841:also
667:Mars
289:The
259:lava
191:and
179:and
173:Mars
44:MOLA
1098:) (
1067:).
843:) (
690:of
2460::
2120:31
1345:.
1299:}}
1295:{{
1102:•
1079:;
847:).
35:.
2436::
2140:2
2130:7
2097:5
1626:)
1622:(
1445:e
1438:t
1431:v
1389:.
1355:.
1330:.
1305:)
1291:.
1106:)
740:.
724:.
342:.
322:.
163:/
160:ə
157:i
154:ʃ
151:ɪ
148:n
145:ˈ
142:ə
139:l
136:p
131:s
128:ɪ
125:n
122:ə
119:z
116:æ
113:m
110:ˈ
107:ə
104:/
100:(
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