Tempe Terra

Tempe Terra is located in the eastern half of the Arcadia quadrangle (MC-03) and the western edge of the Mare Acidalium quadrangle (MC-04) in Mars' western hemisphere. It is centered at {{Coord|39.7|N|289|E|globe:Mars_type:landmark|display=inline,title}} and spans about 2,700 km at its broadest extent. The region extends from about 30° to 54°N and from 265° to 310°E, covering approximately 2.1 million km²,Neesemann, A.; van Gasselt, S; Hauber, E; Neukum, G. (2010) Insights to the Evolution of the Tempe Terra Region, Mars: Refinements of Geologic and Tectonic Units. 41st Lunar and Planetary Science Conference; LPI:Houston, TX, Abstract #2685. {{cite web |url=http://www.lpi.usra.edu/meetings/lpsc2010/pdf/2685.pdf |title=Archived copy |access-date=2011-02-19 |url-status=live |archive-url=https://web.archive.org/web/20110629171659/http://www.lpi.usra.edu/meetings/lpsc2010/pdf/2685.pdf |archive-date=2011-06-29 }}. or an area roughly equivalent to that of Saudi Arabia. It is bordered to the east by Chryse and Acidalia Planitiae, to the north by the low-lying plains of Arcadia and Vastitas Borealis, and to the south by the huge outflow channel system of Kasei Valles.

Tempe Terra occupies a transition zone between the old, heavily cratered highlands of the Martian south and the geologically younger, lowland terrain of the north. Tempe Terra contains the northernmost exposures of ancient highland crust on the planet.Frey, H.V.; Grant, T.D. 1990. Resurfacing History of Tempe Terra and Surroundings. J. Geophys. Res., 95(B9), 14,249–14,263. The region is transected by large numbers of linear to curvilinear normal faults and grabens with ages that span much of Mars' geologic history. Research on extension, or rifts in the crust, has suggested Tempa Terra may be the most highly strained geologic region on Mars{{cite journal | title=Extension across Tempe Terra, Mars, from measurements of fault-scarp widths and deformed craters | url=http://www.agu.org/pubs/crossref/1996/96JE02709.shtml | last=Golombek | first=M.P. | author2=Tanaka, K.L. | author3=Franklin, B.J. | year=1996 | journal=Journal of Geophysical Research: Planets | volume=101 | issue=E11 | page=26119 | doi=10.1029/96JE02709 | bibcode=1996JGR...10126119G | url-status=live | archive-url=https://web.archive.org/web/20121002221733/http://www.agu.org/pubs/crossref/1996/96JE02709.shtml | archive-date=2012-10-02 }} with a lot of low shield volcanoes.

There is evidence of valleys in Tempe Terra, including stream meanders, as in the image below.

ESP 045590 2170hanging.jpg|Hanging valley, as seen by HiRISE under HiWish program This may have been a waterfall at one time.

Image:ESP_025336channels.jpg|Channels, as seen by HiRISE under HiWish program. Stream appears to have eroded through a hill.

File:29054cutoff.jpg|Stream meander and cutoff, as seen by HiRISE under HiWish program.

Martian gullies are small, incised networks of narrow channels and their associated downslope sediment deposits, found on the planet of Mars. They are named for their resemblance to terrestrial gullies. First discovered on images from Mars Global Surveyor, they occur on steep slopes, especially on the walls of craters. Usually, each gully has a dendritic alcove at its head, a fan-shaped apron at its base, and a single thread of incised channel linking the two, giving the whole gully an hourglass shape.Malin, M., Edgett, K. 2000. Evidence for recent groundwater seepage and surface runoff on Mars. Science 288, 2330–2335. They are believed to be relatively young because they have few, if any craters. A subclass of gullies is also found cut into the faces of sand dunes which themselves considered to be quite young.

On the basis of their form, aspects, positions, and location amongst and apparent interaction with features thought to be rich in water ice, many researchers believed that the processes carving the gullies involve liquid water. However, this remains a topic of active research. The pictures below show a variety of gullies and gully features.

Image:ESP_025771variousgullies.jpg|A variety of gullies originating at different levels are visible in this HiRISE image that was taken under the HiWish program.

Image:25771gullybenches.jpg|This enlargement of a small part of the previous image shows terraces along a gully channel. The terraces were created when a new channel cut through the old surface. This means that the gully was not in a single event. Water must have flowed more than once in this location.

Image:ESP_028290_2285gullies.jpg|Gullies in a crater. Some seem to be young, others are well developed. Picture was taken by HiRISE under the HiWish program.

ESP 044707 2285gullies.jpg|Gullies along mesa wall in North Tempe Terra, as seen by HiRISE under HiWish program

44707 2285apron.jpg|Close view of gully apron, as seen by HiRISE under HiWish program Note this is an enlargement of the previous image.

44707 2285alcove.jpg|Close view of gully alcove, as seen by HiRISE under HiWish program Note this is an enlargement of a previous image.

ESP 044852 2285gullies1.jpg|Gullies on wall of mesa, as seen by HiRISE under HiWish program

Linear ridge networks are found in various places on Mars in and around craters.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, 1675-1690. These features have also been called "polygonal ridge networks," "boxwork ridges", and "reticulate ridges."Moore, J., D. Wilhelms. 2001. Hellas as a possible site of ancient ice-covered lakes on Mars. Icarus: 154, 258-276. 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.

ESP 047054 2160ridges.jpg|Wide view of ridge network, as seen by HiRISE under HiWish program

47054 2160largeridges.jpg|Close view of ridge networks, as seen by HiRISE under HiWish program Arrow points to small, straight ridge.

47054 2160largeridgeschanging.jpg|Close view of small and large ridges, as seen by HiRISE under HiWish program

47054 2160smallridges.jpg|Close view of small and large ridges, as seen by HiRISE under HiWish program

Pits and troughs are common on Mars. Large troughs (long narrow depressions) are called fossae in the geographical language used for Mars. This term is derived from Latin; therefore fossa is singular and fossae are plural.{{cite web|url=http://www.marsartgallery.com/marsnames.html|title=Mars Art Gallery Martian Feature Name Nomenclature|website=www.marsartgallery.com|access-date=7 May 2018|url-status=live|archive-url=https://web.archive.org/web/20160724165842/http://www.marsartgallery.com/marsnames.html|archive-date=24 July 2016}} Several mechanisms can form them. Fossae can form 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.Skinner, J., L. Skinner, and J. Kargel. 2007. Re-assessment of Hydrovolcanism-based Resurfacing within the Galaxias Fossae Region of Mars. Lunar and Planetary Science XXXVIII (2007) Studies have found that on Mars a fault may be as deep as 5 km, that is the break in the rock goes down to 5 km. Moreover, the crack or fault sometimes widens or dilates. This widening causes a void to form with a relatively high volume. When surface material slides into the void, a pit crater or a pit crater chain forms. On Mars, individual pit craters can join to form chains or even to form troughs that are sometimes scalloped.Wyrick, D., D. Ferrill, D. Sims, and S. Colton. 2003. Distribution, Morphology and Structural Associations of Martian Pit Crater Chains. Lunar and Planetary Science XXXIV (2003)

File:ESP 053754 2125lineofpits.jpg|Line of pits, as seen by HiRISE under HiWish program Fossae often seem to start with a line of pits.

File:ESP 053886 2145bigpits.jpg|Pits in shallow trough, as seen by HiRISE under HiWish program

File:ESP 053805 2140troughs.jpg|Troughs (Fossae), as seen by HiRISE under HiWish program

The pictures below are probably formed from ice. The Martian surface displays many differed types of holes, pits, depressions, and hollows that are believed to have been caused by large amounts of ice disappearing from the ground. When the ice leaves, the ground collapses. Because of the thin atmosphere on the planet, the ice sublimates—goes directly from a solid phase to a gas phase. Dry ice does that on the Earth. Eskers form when a stream runs under a glacier and deposits material that is left behind when the glacier disappears.

File:Tempe Terra.jpg|Tempe Terra as seen in MOLA colorized image. Red areas show highest elevations; blue, lowest. Acidalia Planitia is the blue area at extreme right. The immense outflow channels of Kasei Valles is in the lower right.

File:ESP 028672 2235hollows.jpg|Hollows formed by erosion on floor of crater, as seen by HiRISE under HiWish program

Image:23503esker.jpg|Esker, as seen by HiRISE under the HiWish program.

ESP 043824 2180layers.jpg|Layers, as seen by HiRISE under HiWish program Location is Tempe Terra in Arcadia quadrangle.

43824 2160layers.jpg|Layers, as seen by HiRISE under HiWish program Location is Tempe Terra Note: this is an enlargement of the previous image.

• Climate on Mars
• Glaciers
• Glaciers on Mars
• Martian Gullies
• Water on Mars

{{reflist|colwidth=30em}}

{{commons category|Tempe Terra}}

• [https://www.youtube.com/watch?v=_sUUKcZaTgA Martian Ice - Jim Secosky - 16th Annual International Mars Society Convention]
• [http://www.esa.int/SPECIALS/Mars_Express/SEM8LI8ATME_0.html Mars Express]
• [http://hiroc.lpl.arizona.edu/images/PSP/PSP_001390_2290/ HiRISE image of a hill in Tempe Terra]

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Category:Terrae on Mars

Category:Arcadia quadrangle

Category:Mare Acidalium quadrangle