MOLA colorized relief map of Amazonis Planitia, the type area for the Amazonian System. Note that Amazonis Planitia is characterized by low rates of meteorite and asteroid impacts. Colors indicate elevation, with red highest, yellow intermediate, and green/blue lowest.

The Amazonian is a geologic system and early time period on the planet Mars characterized by low rates of meteorite and asteroid impacts and by cold, hyperarid conditions broadly similar to those on Mars today.^[1][2] The transition from the preceeding Hesperian period is transitional and somewhat poorly defined. The Amazonian is thought to have begun around 3 billion years ago, though error bars on this date are extremely large (~500 million years).^[3] The period is sometimes subdivided into the Early, Middle, and Late Amazonian. The Amazonian continues to the present day.

Description and name origin [link]

The Amazonian System and Period is named after Amazonis Planitia, which has a sparse crater density over a wide area. Such densities are representative of many Amazonian-aged surfaces. The type area of the Amazonian System is in the Amazonis quadrangle (MC-8) around {{#invoke:Coordinates|coord}}{{#coordinates:15|N|158|W|globe:Mars|||| | |name= }}.

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TimeAxis = orientation:horizontal ScaleMajor = unit:year increment:500 start:-4500 ScaleMinor = unit:year increment:100 start:-4500

Colors=

id:prenoachicol value:rgb(0.7,0.4,1)
id:noachicol value:rgb(0.5,0.5,0.8)
id:hespericol value:rgb(1,0.2,0.2)
id:amazonicol value:rgb(1,0.5,0.2)

PlotData=

align:center textcolor:black fontsize:8 mark:(line,black) width:25 shift:(0,-5)
text:Amazonian from:-3000 till:0 color:amazonicol
text:Hesperian from:-3700 till:-3000 color:hespericol
text:Noachian from:-4100 till:-3700 color:noachicol
text:Pre-Noachian from:start till:-4100 color:prenoachicol

</timeline>

[edit] Amazonian chronology and stratigraphy

HiRISE image illustrating superpositioning, a principle that lets geologists determine the relative ages of surface units. The dark-toned lava flow overlies (is younger than) the light-toned, more heavily cratered terrain (older lava flow?) at right. The ejecta of the crater at center overlies both units, indicating that the crater is the youngest feature in the image.

Because it is the youngest of the Martian periods, the chronology of the Amazonian is comparatively well understood through traditional geological laws of superposition coupled to the relative dating technique of crater counting. The scarcity of craters characteristic of the Amazonian also means that unlike the older periods, fine scale (<100 m) surface features are preserved.^[4] This enables detailed, process-orientated study of many Amazonian-age surface features of Mars as the necessary details of form of the surface are still visible.

Furthermore, the relative youth of this period means that over the past few 100 million years it remains possible to reconstruct the statistics of the orbital mechanics of the Sun, Mars, and Jupiter without the patterns being overwhelmed by chaotic effects, and from this to reconstruct the variation of solar insolation - the amount of heat from the sun - reaching Mars through time.^[5] Climatic variations have been shown to occur in cycles not dissimilar in magnitude and duration to terrestrial Milankovich cycles.

Together, these features - good preservation, and an understanding of the imposed solar flux - mean that much research on the Amazonian of Mars has focussed on understanding its climate, and the surface processes that respond to the climate. This has included:

• glacial dynamics and landforms,^[6]
• the advance and retreat of ice across the planet,^[7]
• the behavior of ground ice and the periglacial forms which it produces,^[8]
• melt processes and small scale fluvial geomorphology,^[9]
• variation in atmospheric properties,^[10]
• groundwater dynamics,^[11]
• ice cap dynamics,^[12]
• CO₂ frost dynamics, and exotic surface features related to them such as "spiders"^[13]
• the effects of wind on deposits of sand and dust and general aeolian sedimentology,^[14][15]
• and the modelling of past climate conditions (wind fields, temperatures, cloud properties, atmospheric chemistry) themselves.^[16][17]

Good preservation has also enabled detailed studies of other geological processes on Amazonian Mars, notably volcanic processes,^[18][19][20] brittle tectonics,^[21][22] and cratering processes.^[23][24][25]

System vs. Period [link]

System and Period are not interchangeable terms in formal stratigraphic nomenclature, although they are frequently confused in popular literature. A system is an idealized stratigraphic column based on the physical rock record of a type area (type section) correlated with rocks sections from many different locations planetwide.^[27] A system is bound above and below by strata with distinctly different characteristics (on Earth, usually index fossils) that indicate dramatic (often abrupt) changes in the dominant fauna or environmental conditions. (See Cretaceous–Paleogene boundary as example.)

At any location, rock sections in a given system are apt to contain gaps (unconformities) analogous to missing pages from a book. In some places, rocks from the system are absent entirely due to nondeposition or later erosion. For example, rocks of the Cretaceous System are absent throughout much of the eastern central interior of the United States. However, the time interval of the Cretaceous (Cretaceous Period) still occurred there. Thus, a geologic period represents the time interval over which the strata of a system were deposited, including any unknown amounts of time present in gaps.^[27] Periods are measured in years, determined by radioactive dating. On Mars, radiometric ages are not available except from Martian meteorites whose provenance and stratigraphic context are unknown. Instead, absolute ages on Mars are determined by impact crater density, which is heavily dependent upon models of crater formation over time.^[28] Accordingly, the beginning and end dates for Martian periods are uncertain, especially for the Hesperian/Amazonian boundary, which may be in error by a factor of 2 or 3.^[29][30]

Images [link]

• 

  Pedestal crater in Amazonis with Dark Slope Streaks, as seen by HiRISE.

• Tooting Crater.JPG

  Wall of Tooting Crater, as seen by HiRISE.

• Pettit Crater Rim.JPG

  Pettit Crater rim, as seen by HiRISE.

• Nicholson Crater Mound.JPG

  Nicholson mound with dark streaks, as seen by HiRISE.

• Lycus Sulci.JPG

  Lycus Sulci, as seen by HiRISE.

• Marte Vallis Island.JPG

  Streamlined Island in Marte Vallis, as seen by HiRISE.

• Tartarus Colles Channel.JPG

  Tartarus Colles channel, as seen by HiRISE.

• 

  Channels From Fissure, as seen by HiRISE.

• 

  Narrow ridges, as seen by HiRISE.

• 

  Plateau made up of Medusae Fossae materials and rootless cones, as seen by HiRISE.

• 

  Surfaces in Amazonis quadrangle, as seen by HiRISE.

See also [link]

• Geological history of Mars
• Geology of Mars

Notes and references [link]

Bibliography and recommended reading [link]

• Boyce, Joseph, M. (2008). The Smithsonian Book of Mars; Konecky & Konecky: Old Saybrook, CT, ISBN 978-1-58834-074-0
• Carr, Michael, H. (2006). The Surface of Mars; Cambridge University Press: Cambridge, UK, ISBN 978-0-521-87201-0.
• Hartmann, William, K. (2003). A Traveler’s Guide to Mars: The Mysterious Landscapes of the Red Planet; Workman: New York, ISBN 0-7611-2606-6.
• Morton, Oliver (2003). Mapping Mars: Science, Imagination, and the Birth of a World; Picador: New York, ISBN 0-312-42261-X.

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