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Amenthes quadrangle

Coordinates: 15°00′N 247°30′W / 15°N 247.5°W / 15; -247.5
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Amenthes quadrangle
Map of Amenthes quadrangle from Mars Orbiter Laser Altimeter (MOLA) data. The highest elevations are red and the lowest are blue.
Coordinates15°00′N 247°30′W / 15°N 247.5°W / 15; -247.5
Image of the Amenthes Quadrangle (MC-14). The southern part includes heavily cratered highlands; the northern part contains Elysium Planitia; and the eastern half includes Isidis basin.

The Amenthes quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS) Astrogeology Research Program. The Amenthes quadrangle is also referred to as MC-14 (Mars Chart-14).[1] The quadrangle covers the area from 225° to 270° west longitude and from 0° to 30° north latitude on Mars. Amenthes quadrangle contains parts of Utopia Planitia, Isidis Planitia, Terra Cimmeria, and Tyrrhena Terra.

The name Amenthes is the Egyptian word for the place where the souls of the dead go.[2]

This quadrangle contains the Isidis basin, a location where magnesium carbonate was found by MRO. This mineral indicates that water was present and that it was not acidic. There are Dark slope streaks, troughs (fossae), and river valleys (Vallis) in this quadrangle.

The Beagle 2 lander was about to land in the quadrangle, particularly in the eastern part of Isidis Planitia, in December 2003, when contact with the craft was lost. In January 2015, NASA reported the Beagle 2 had been found on the surface in Isidis Planitia (location is about 11°31′35″N 90°25′46″E / 11.5265°N 90.4295°E / 11.5265; 90.4295).[3][4] High-resolution images captured by the Mars Reconnaissance Orbiter identified the lost probe, which appears to be intact.[5][6][7] (see discovery images here)

Craters

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Some craters in the Amenthes region (as well as other parts of Mars) show ejecta around them that have lobes. It is believed that the lobed shape is caused by an impact into water or ice logged ground. Calculations suggest that ice is stable beneath the Martian surface.

At the equator the stable layer of ice might lie under as much as 1 kilometer of material, but at higher latitudes the ice may be just a few centimeters below the surface. This was proven when the landing rockets on the Phoenix lander blew away surface dust to reveal an ice surface.[8][9] The larger an impact crater, the deeper its penetration, a large crater is more likely to have a lobate ejecta since it went down to the ice layer. When even small craters have lobes, the ice level is close to the surface.[10] This idea would be very important for future colonists on Mars who would like to live near a source of water.

Impact craters generally have a rim with ejecta around them, in contrast volcanic craters usually do not have a rim or ejecta deposits.[11] Sometimes craters will display layers. Since the collision that produces a crater is like a powerful explosion, rocks from deep underground are tossed unto the surface. Hence, craters can show us what lies deep under the surface. One crater in the Amenthes quadrangle is believed to be a source of nakhlite meteorites. A team of researchers found that these particular meteorites came from four different eruptions of lava because they showed different ages. The ages were measured by comparing isotopes of the element argon. Since the ages vary from 93 to 1322 million years, the authors concluded that volcanoes grow much more slowly on Mars than the Earth. Many of the volcanoes on the Earth grow much quicker, as they form at plate boundaries. In contrast, Martian volcanoes probably form from plumes.[12]

  • Escalante Crater wall, as seen by HiRISE. Image on left is an enlargement.
    Escalante Crater wall, as seen by HiRISE. Image on left is an enlargement.
  • Onon Crater, as seen by HiRISE. Scale bar is 500 meters long.
    Onon Crater, as seen by HiRISE. Scale bar is 500 meters long.
  • Libya Montes Region, as seen by HiRISE. Image contains some sheer rock cliffs.
    Libya Montes Region, as seen by HiRISE. Image contains some sheer rock cliffs.
  • Western side of Du Martheray Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter)
    Western side of Du Martheray Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter)
  • Crater and ejecta, as seen by HiRISE under HiWish program
    Crater and ejecta, as seen by HiRISE under HiWish program
  • Close view of crater and ejecta, as seen by HiRISE under HiWish program
    Close view of crater and ejecta, as seen by HiRISE under HiWish program
  • Close view of crater ejecta, as seen by HiRISE under HiWish program
    Close view of crater ejecta, as seen by HiRISE under HiWish program
  • Rocks at crater rim, as seen by HiRISE under HiWish program
    Rocks at crater rim, as seen by HiRISE under HiWish program

Hebrus Valles

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Hebrus Vales has tributaries, terraces, and teardrop shaped islands. The tear drop shape of the islands indicate what direction the water used to flow. The terraces may be caused by different layers of rocks or from the water being at different levels.[13] These features are common for the rivers of the Earth.

  • Hebrus Valles, as seen by THEMIS. Direction of flow was determined by shape of streamlined islands. Terraces may have been due to separate flood events.
    Hebrus Valles, as seen by THEMIS. Direction of flow was determined by shape of streamlined islands. Terraces may have been due to separate flood events.
  • Hebrus Valles, as seen from Themis. Since discontinuous pits and troughs are present, collapse of material into a void may have caused the troughs.
    Hebrus Valles, as seen from Themis. Since discontinuous pits and troughs are present, collapse of material into a void may have caused the troughs.

Streamlined shapes

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Streamlined shapes are formed from erosion by flowing water.

  • Wide view of streamlined shapes, as seen by HiRISE under HiWish program
    Wide view of streamlined shapes, as seen by HiRISE under HiWish program
  • Close view of streamlined shapes, as seen by HiRISE under HiWish program. Arrow indicates the direction of past flowing water.
    Close view of streamlined shapes, as seen by HiRISE under HiWish program. Arrow indicates the direction of past flowing water.
  • Close view of streamlined shapes, as seen by HiRISE under HiWish program
    Close view of streamlined shapes, as seen by HiRISE under HiWish program
  • Close view of streamlined shapes, as seen by HiRISE under HiWish program
    Close view of streamlined shapes, as seen by HiRISE under HiWish program
  • Streamlined shapes formed by flowing water, as seen by HiRISE under HiWish program
    Streamlined shapes formed by flowing water, as seen by HiRISE under HiWish program

Cones

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  • Wide view of cones and trough, as seen by HiRISE under HiWish program
    Wide view of cones and trough, as seen by HiRISE under HiWish program
  • Cone next to a trough, as seen by HiRISE under HiWish
    Cone next to a trough, as seen by HiRISE under HiWish
  • Cones, as seen by HiRISE under HiWish
    Cones, as seen by HiRISE under HiWish
  • Line of cones, as seen by HiRISE under HiWish program
    Line of cones, as seen by HiRISE under HiWish program
  • Cones, as seen by HiRISE under HiWish program. White arrows point to some of the cones.
    Cones, as seen by HiRISE under HiWish program. White arrows point to some of the cones.

Mesas

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Mesas form when erosion has removed much of the surrounding ground. They are the remains of material that once covered a wide area.

  • Layered mesa that appears to have a streamlined shape, as seen by HiRISE under HiWish program. A channel has cut through a lower layer.
    Layered mesa that appears to have a streamlined shape, as seen by HiRISE under HiWish program. A channel has cut through a lower layer.
  • Layered mesa, as seen by HiRISE under HiWish program
    Layered mesa, as seen by HiRISE under HiWish program

Fossae

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The Amenthes quadrangle is also home to troughs (long narrow depressions) called fossae in the geographical language used for Mars. These troughs form when the crust is stretched until it breaks. The stretching can be due to the large weight of a nearby volcano.

  • Wall of trough of Amenthes Fossae, as seen by HiRISE under HiWish program
    Wall of trough of Amenthes Fossae, as seen by HiRISE under HiWish program
  • Large pits, as seen by HiRISE under HiWish program
    Large pits, as seen by HiRISE under HiWish program
  • Trough, as seen by HiRISE under HiWish program
    Trough, as seen by HiRISE under HiWish program
  • Hephaestus Fossae Two Views, as seen by HiRISE. Picture on right lies to the top (north) of other picture. Fossa often form by material moving into an underground void.
    Hephaestus Fossae Two Views, as seen by HiRISE. Picture on right lies to the top (north) of other picture. Fossa often form by material moving into an underground void.
  • Troughs, as seen by HiRISE under HiWish program
    Troughs, as seen by HiRISE under HiWish program
  • Troughs cutting through mesa, as seen by HiRISE under HiWish program
    Troughs cutting through mesa, as seen by HiRISE under HiWish program

Channels

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  • Group of channels, as seen by HiRISE under HiWish program
    Group of channels, as seen by HiRISE under HiWish program
  • Granicus Vallis Tributary, as seen by HiRISE
    Granicus Vallis Tributary, as seen by HiRISE
  • Channels, as seen by HiRISE under HiWish program
    Channels, as seen by HiRISE under HiWish program

Other landscape features

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  • Map of Amenthes quadrangle. The northwest part includes Isidis Planitia. Escalante Crater is near the equator.
    Map of Amenthes quadrangle. The northwest part includes Isidis Planitia. Escalante Crater is near the equator.
  • Lobate ejecta in Amenthes. Large crater has lobate ejecta, smaller craters do not show such ejecta since the ice layer was not penetrated by the smaller impacts.
    Lobate ejecta in Amenthes. Large crater has lobate ejecta, smaller craters do not show such ejecta since the ice layer was not penetrated by the smaller impacts.
  • Tinjar Vallis, as seen by THEMIS. Color is enhanced to show differences.
    Tinjar Vallis, as seen by THEMIS. Color is enhanced to show differences.
  • Scamander Vallis. Dark slope streaks may be seen in the image. The darker the streak, the younger it is.
    Scamander Vallis. Dark slope streaks may be seen in the image. The darker the streak, the younger it is.

Other Mars quadrangles

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Mars Quad Map
Mars Quad Map
The image above contains clickable linksClickable image of the 30 cartographic quadrangles of Mars, defined by the USGS.[14][15] Quadrangle numbers (beginning with MC for "Mars Chart")[16] and names link to the corresponding articles. North is at the top; 0°N 180°W / 0°N 180°W / 0; -180 is at the far left on the equator. The map images were taken by the Mars Global Surveyor.
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Interactive Mars map

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Map of MarsAcheron FossaeAcidalia PlanitiaAlba MonsAmazonis PlanitiaAonia PlanitiaArabia TerraArcadia PlanitiaArgentea PlanumArgyre PlanitiaChryse PlanitiaClaritas FossaeCydonia MensaeDaedalia PlanumElysium MonsElysium PlanitiaGale craterHadriaca PateraHellas MontesHellas PlanitiaHesperia PlanumHolden craterIcaria PlanumIsidis PlanitiaJezero craterLomonosov craterLucus PlanumLycus SulciLyot craterLunae PlanumMalea PlanumMaraldi craterMareotis FossaeMareotis TempeMargaritifer TerraMie craterMilankovič craterNepenthes MensaeNereidum MontesNilosyrtis MensaeNoachis TerraOlympica FossaeOlympus MonsPlanum AustralePromethei TerraProtonilus MensaeSirenumSisyphi PlanumSolis PlanumSyria PlanumTantalus FossaeTempe TerraTerra CimmeriaTerra SabaeaTerra SirenumTharsis MontesTractus CatenaTyrrhena TerraUlysses PateraUranius PateraUtopia PlanitiaValles MarinerisVastitas BorealisXanthe Terra
The image above contains clickable linksInteractive image map of the global topography of Mars. Hover your mouse over the image 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.


See also

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References

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  1. ^ Davies, M.E.; Batson, R.M.; Wu, S.S.C. “Geodesy and Cartography” in Kieffer, H.H.; Jakosky, B.M.; Snyder, C.W.; Matthews, M.S., Eds. Mars. University of Arizona Press: Tucson, 1992.
  2. ^ Blunck, J. 1982. Mars and its Satellites. Exposition Press. Smithtown, N.Y.
  3. ^ Ellison, Doug (16 January 2015). "re Beagle 2 location on Mars => "Using HiView on image ESP_039308_1915_COLOR.JP2 I get 90.4295E 11.5265N"". Twitter & JPL. Retrieved 19 January 2015.
  4. ^ Grecicius, Tony; Dunbar, Brian (16 January 2015). "Components of Beagle 2 Flight System on Mars". NASA. Retrieved 18 January 2015.
  5. ^ Webster, Guy (16 January 2015). "'Lost' 2003 Mars Lander Found by Mars Reconnaissance Orbiter". NASA. Retrieved 16 January 2015.
  6. ^ "Mars Orbiter Spots Beagle 2, European Lander Missing Since 2003". The New York Times. Associated Press. 16 January 2015. Retrieved 17 January 2015.
  7. ^ Amos, Jonathan (16 January 2015). "Lost Beagle2 probe found 'intact' on Mars". BBC. Retrieved 16 January 2015.
  8. ^ NASA.gov
  9. ^ NASA.gov[dead link‍]
  10. ^ "ESA Science & Technology - Science Portal".
  11. ^ Hugh H. Kieffer (1992). Mars. University of Arizona Press. ISBN 978-0-8165-1257-7. Retrieved 7 March 2011.
  12. ^ Cohen, B., et al. 2017. Taking the pulse of Mars via dating of a plume-fed volcano. Nature Communications. 8, 640.
  13. ^ "Hebrus Valles | Mars Odyssey Mission THEMIS".
  14. ^ Morton, Oliver (2002). Mapping Mars: Science, Imagination, and the Birth of a World. New York: Picador USA. p. 98. ISBN 0-312-24551-3.
  15. ^ "Online Atlas of Mars". Ralphaeschliman.com. Retrieved 16 December 2012.
  16. ^ "PIA03467: The MGS MOC Wide Angle Map of Mars". Photojournal. NASA / Jet Propulsion Laboratory. 16 February 2002. Retrieved 16 December 2012.
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