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The Olympica Fossae are a set of troughs in the Tharsis quadrangle of Mars at 25° north latitude and 114.1° west longitude. They are about 420 km long and were named after an albedo feature at 17N, 134W.[1] Parts of the fossae have been suggested to be both outflow channels as well as channels for flowing lava, routing both molten rock and catastrophic outburst floods of water at different times in Mars' geological past.[2]

Olympica Fossae
Olympica Fossae based on THEMIS Day IR.png
Image of the Olympica Fosae based on THEMIS day-time image
Coordinates25°00′N 114°06′W / 25°N 114.1°W / 25; -114.1Coordinates: 25°00′N 114°06′W / 25°N 114.1°W / 25; -114.1
Map of Tharsis quadrangle with major features indicated. Tharsis contains many volcanoes, including Olympus Mons, the tallest known volcano in the solar system. Notice Ceraunius Tholus, although it looks small, it is about as high as Earth's Mount Everest.

Contents

FossaEdit

The Olympica Fossae are a large set of troughs, called fossae in the geographical language used for Mars. Troughs form when the crust is stretched until it breaks along two subparallel failure planes, or faults. The middle section between the faults moves down, forming the trough and leaving steep cliffs along the sides. Sometimes, a line of pits form as material collapse into a void that forms from the stretching. Such fault-bounded geological structures are also called graben.[3]

Dark slope streaksEdit

A picture below shows dark streaks on the Olympica Fossae. Such streaks are common on Mars. They occur on steep slopes of craters, troughs, and valleys. The streaks are dark at first. They get lighter with age. Sometimes they start in a tiny spot, then spread out and go for hundreds of meters. They have been seen to travel around obstacles, like boulders.[4] It is believed that they are avalanches of bright dust that expose a darker underlying layer. However, several ideas have been advanced to explain them. Some involve water or even the growth of organisms.[5][6][7] The streaks appear in areas covered with dust. Much of the Martian surface is covered with dust. Fine dust settles out of the atmosphere covering everything. We know a lot about this dust because the solar panels of the Mars Rovers get covered with dust, thus reducing the electrical energy. The power of the Rovers has been restored many times by the wind, in the form of dust devils, cleaning the panels and boosting the power.[8] Dust storms 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 then the Earth's. That is the difference between the farthest point from the sun and the closest point to the sun is very great for Mars, but only a slight amount for the Earth. Also, every few years, the entire planet is engulfed in global dust storms. When NASA's Mariner 9 craft arrived there, nothing could be seen through the dust storm.[9][10] Other global dust storms have also been observed, since that time.

Interactive Mars mapEdit

Acheron FossaeAcidalia PlanitiaAlba MonsAmazonis PlanitiaAonia PlanitiaArabia TerraArcadia PlanitiaArgentea PlanumArgyre PlanitiaChryse PlanitiaClaritas FossaeCydonia MensaeDaedalia PlanumElysium MonsElysium PlanitiaGale craterHadriaca PateraHellas MontesHellas PlanitiaHesperia PlanumHolden craterIcaria PlanumIsidis PlanitiaJezero craterLucus PlanumLycus SulciLunae PlanumLyot craterMalea PlanumMaraldi craterMareotis FossaeMareotis TempeMargaritifer TerraMie craterMilankovič craterMoreux craterNepenthes MensaeNereidum MontesNilosyrtis MensaeNoachis TerraOlympica FossaeOlympus MonsPlanum AustralePromethei TerraProtonilus MensaeSirenumSisyphi PlanumSolis PlanumSyria PlanumTantalus FossaeTempe TerraTerra CimmeriaTerra SabaeaTerra SirenumTharsis MontesTractus CatenaTyrrhen TerraUlysses PateraUranius PateraUtopia PlanitiaValles MarinerisVastitas BorealisXanthe Terra 
 Interactive imagemap of the global topography of Mars. Hover your mouse to see the names of over 60 prominent geographic features, and click to link to them. Coloring of the base map indicates relative elevations, based on data from the Mars Orbiter Laser Altimeter on NASA's Mars Global Surveyor. Whites and browns indicate the highest elevations (+12 to +8 km); followed by pinks and reds (+8 to +3 km); yellow is 0 km; greens and blues are lower elevations (down to −8 km). Axes are latitude and longitude; Polar regions are noted.


ReferencesEdit

  1. ^ http://planetarynames.wr.usgs.gov
  2. ^ Carr, M.H. (2006), The Surface of Mars. Cambridge Planetary Science Series, Cambridge University Press.
  3. ^ http://www.msss.com/mars_images/moc/2004/01/29/index.html
  4. ^ http://www.space.com/image_of_day_080730.html
  5. ^ http://www.spcae.com/scienceastronomy/streaks_mars_021211.html
  6. ^ http://www.space.com/scienceastronomy/streaks_mars_streaks_030328.html
  7. ^ http://www.space.com/scienceastronomy/mars_
  8. ^ https://www.sciencedaily.com/releases/2009/02/090217101110.htm
  9. ^ ISBN 0-517-00192-6
  10. ^ Hugh H. Kieffer (1992). Mars. University of Arizona Press. ISBN 978-0-8165-1257-7. Retrieved 7 March 2011.

See alsoEdit