“Tempe Terra”的意思、由来-开放百科全书

Tempe Terra is a heavily cratered highland region in the northern hemisphere of the planet Mars. Located at the northeastern edge of the Tharsis volcanic province, Tempe Terra is notable for its high degree of crustal fracturing and deformation. The region also contains a large number of small shield volcanoes, lava flows, and other volcanic structures.

The region is named after the albedo feature Tempe, first used by astronomer E.M. Antoniadi in 1930 to describe a bright patch of terrain centered near 40°N, 70°W. The name comes from the Vale of Tempe, a valley located south of Mount Olympus and celebrated by the ancient Greeks for its beauty. The International Astronomical Union (IAU) formally designated the region Tempe Terra in 1979. Terra (pl. terrae) is a Latin descriptor term used in planetary geology for continent-like highland regions (i.e., extensive land masses) on other planets.^[1]

Location and description

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.^[1] The region extends from about 30° to 54°N and from 265° to 310°E, covering approximately 2.1 million km²,^[2] 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.

Geology

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.^[3] 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^[4] with a lot of low shield volcanoes.

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

Gullies

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.^[5] 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.

Linear ridge networks

Linear ridge networks are found in various places on Mars in and around craters.^[6] These features have also been called "polygonal ridge networks," "boxwork ridges", and "reticulate ridges."^[7] 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.

Pits and troughs

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.^[8] 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.^[9] 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.^[10]

Other images from Tempe Terra

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.

Interactive Mars map

See also

References

1. ^¹Gazetteer of Planetary Nomenclature. http://planetarynames.wr.usgs.gov {{webarchive|url=https://web.archive.org/web/20160331045425/http://planetarynames.wr.usgs.gov/ |date=2016-03-31 }}.
2. ^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 |accessdate=2011-02-19 |deadurl=no |archiveurl=https://web.archive.org/web/20110629171659/http://www.lpi.usra.edu/meetings/lpsc2010/pdf/2685.pdf |archivedate=2011-06-29 |df= }}.
3. ^Frey, H.V.; Grant, T.D. 1990. Resurfacing History of Tempe Terra and Surroundings. J. Geophys. Res., 95(B9), 14,249–14,263.
4. ^{{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 | deadurl=no | archiveurl=https://web.archive.org/web/20121002221733/http://www.agu.org/pubs/crossref/1996/96JE02709.shtml | archivedate=2012-10-02 | df= }}
5. ^Malin, M., Edgett, K. 2000. Evidence for recent groundwater seepage and surface runoff on Mars. Science 288, 2330–2335.
6. ^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.
7. ^Moore, J., D. Wilhelms. 2001. Hellas as a possible site of ancient ice-covered lakes on Mars. Icarus: 154, 258-276.
8. ^{{cite web|url=http://www.marsartgallery.com/marsnames.html|title=Mars Art Gallery Martian Feature Name Nomenclature|author=|date=|website=www.marsartgallery.com|accessdate=7 May 2018|deadurl=no|archiveurl=https://web.archive.org/web/20160724165842/http://www.marsartgallery.com/marsnames.html|archivedate=24 July 2016|df=}}
9. ^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)
10. ^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)