- Syrtis Major
MarsGeo-Mount
name=Syrtis Major
caption=Mars digital-image mosaic merged with color of the MC-13 quadrangle, Syrtis Major region of Mars.
location=
latitude=8.4
N_or_S=N
longitude=69.5
E_or_W=E
peak=
discoverer=
eponym=Syrtis Major Planum is a "dark spot" (an
albedo feature ) located in the boundary between the northern lowlands and southern highlands of Mars. It was discovered, on the basis of data fromMars Global Surveyor , to be a low-reliefshield volcano Citation
last = Hiesinger
first = H.
author-link =
last2 = Head ( [http://www.planetary.brown.edu/html_pages/headpubs.htm publications] )
first2 = J. W.
author2-link =
title = The Syrtis Major volcanic province, Mars: Synthesis from Mars Global Surveyor data
journal = Journal of Geophysical Research
volume = 109
issue = E1
date =2004-01-08
year = 2004
url = http://www.planetary.brown.edu/pdfs/2763.pdf
doi = 10.1029/2003JE002143
id = E01004
pages = E01004] , but was formerly believed to be aplain , and was then known as Syrtis Major Planitia. The dark color comes from thebasalt ic volcanic rock of the region and the relative lack of dust.Geography and geology
Syrtis Major is centered near at coord|8.4|69.5|globe:Mars, extends some 1,500 km (930 miles) north from the planet's equator, and spans 1,000 km (620 miles) from west to east. It encompasses a large slope from its western edge at
Aeria dropping 4 km (2.5 miles) to its eastern edge atIsidis Planitia . It includes a high-altitude bulge that rises 6 km (3.7 miles) at 310° W. Most of Syrtis Major has slopes of less than 1°, a much lower inclination than the slopes of theTharsis shield volcanoes. It has a 350x150 km north-south elongated central depression containing thecaldera sNili Patera andMeroe Patera , which are about 2 km deep. The floors of the calderas are not elevated relative to the terrain surrounding Syrtis Major. The floor of Nili Patera is the less cratered, and therefore the younger, of the two. While most of the rock is basaltic,dacite has also been detected in Nili Patera.cite web
title = Mars Odyssey Mission THEMIS web site
date = 2006-10-23
url = http://themis.asu.edu/features/nilipatera
accessdate = 2007-09-08 ] Satellite gravity field measurements show a positive gravity anomaly centered on the caldera complex, inferring the presence of a 600x300 km north-south elongated extinctmagma chamber below, containing dense minerals (probably mainlypyroxene , witholivine also possible) that precipitated out ofmagma before eruptions. [cite journal
last = Kiefer
first = Walter S.
title = Gravity evidence for an extinct magma chamber beneath Syrtis Major, Mars: a look at the magmatic plumbing system
journal = Earth and Planetary Science Letters
volume = 222
issue = 2
pages = 349– 361
date =2004-05-30
doi = 10.1016/j.epsl.2004.03.009] Crater counts date Syrtis Major to the early Hesperian epoch; it postdates formation of the adjacent Isidisimpact basin .Discovery and name
The name Syrtis Major is derived from the classical Roman name "Syrtis maior" for the
Gulf of Sidra on the coast ofLibya (classicalCyrenaica ).Syrtis Major was the first documented surface feature of another
planet . It was discovered byChristiaan Huygens , who included it in a drawing of Mars in1659 . The feature was originally known as the Hourglass Sea but has been given different names by differentcartographer s. In 1840,Johann von Mädler compiled a map of Mars from his observations and called the feature Atlantic Canale. InRichard Proctor 's1867 map it is called then Kaiser Sea (afterFrederick Kaiser of theLeiden Observatory ).Camille Flammarion called it the Mer du Sablier (French for "Hourglass Sea") when he revised Proctor's nomenclature in1876 . The name "Syrtis Major" was chosen byGiovanni Schiaparelli when he created a map based on observations made during Mars' close approach to Earth in 1877. [cite book| title=Mapping Mars: Science, Imagination, and the Birth of a World| first=Oliver| last=Morton| publisher=Picador USA| location=New York| year=2002| isbn=0312245513| pages=14-15] [cite web|url=http://www.uapress.arizona.edu/onlinebks/mars/chap04.htm|title=The Planet Mars: A History of Observation and Discovery - Chapter 4: Areographers|author=William Sheehan|accessdate=2007-09-07]easonal variations
Syrtis Major was the object of much observation due to its seasonal and long-term variations. This led to theories that it was a shallow sea and later that its variability was due to seasonal vegetation. However, in the 1960s and 1970s, the Mariner and Viking planetary probes led scientists to conclude that the variations were caused by wind blowing dust and sand across the area. It has many windblown deposits that include light-colored halos or "
plumose streaks " that form downwind of craters. These streaks are accumulations of dust resulting from disruption of the wind by the elevated rims of the craters ('wind shadows').References
ee also
*
List of mountains on Mars by height External links
* [http://www.google.com/mars/#lat=11.178401&lon=66.181640&zoom=4&
]
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