Mare Tyrrhenum quadrangle

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Mars topography (MOLA dataset) HiRes (1).jpg
MC-22 Mare Tyrrhenum 0–30° S 90–135° E Quadrangles Atlas

The Mare Tyrrhenum quadrangle contains a rich variety of features that include one of the planet’s oldest volcanoes, and many of the usual beautiful landscapes on the planet such as columnar jointing, craters, dunes, ridge networks, and even a landslide. In this article, some of the best pictures from a number of spacecraft will show what the landscape looks like in this region. The origins and significance of all features will be explained as they are currently understood.

Geography and origin of name

Most of the region contains heavily cratered highlands. The central part contains Tyrrhena Patera (a very old volcano). The Mare Tyrrhenum quadrangle encompasses parts of the regions Tyrrhena Terra, Hesperia Planum, and Terra Cimmeria. Mare Tyrrhenum's largest crater is Herschel. Licus Vallis and the Ausonia Montes are other major features in the region. The Mare Tyrrhenum quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS). This quadrangle is also referred to as MC-22 (Mars Chart-22).[1] This quadrangle covers the area from 0° to 30° south latitude and 225° to 270° west longitude (135-90 E). Giovanni Schiaparelli named the area after Earth's Tyrrhenian Sea, which lies between Italy and Sicily. The region was subsequently renamed to Mare Tyrrhena after spacecraft photos revealed that it is an old, cratered plain rather than a sea.[2] [3]

Importance of craters

The density of impact craters is used to determine the surface ages of Mars and other solar system bodies.[4] The older the surface, the more craters present. The floors of many craters have dunes. Dunes form in them because wind on Mars is not strong enough to lift sand grains all the way out of a crater. The Mare Tyrrhenum quadrangle lies in the southern hemisphere—an old region with many craters. The area around craters may be rich in minerals. On Mars, heat from an impact melts ice in the ground. Water from the melting ice dissolves minerals, and then deposits them in cracks or faults that were produced with the impact. This process, called hydrothermal alteration, is a major way in which ore deposits are produced. Perhaps this process will have made the area around Martian craters rich in useful ores for the future colonization of Mars.[5]

Close-up of depression on crater floor Rectangle represents the size of a football field. Close-up of depression on crater floor, as seen by HiRISE under HiWish program. Rectangle represents the size of a football field.


Hydrothermal features in Auki

The crater Auki shows ridge networks that some researchers believe to be evidence of hydrothermal processes that occurred after impact. Impacts fracture rock and create enormous amounts of heat. On Mars, this heat can cause ice to melt and then force the resulting water to move through cracks that were generated during impact. This water will eventually deposit minerals. Mineral deposits may become evident when surrounding ground erodes. Deposits formed in this manner are more resistant to erosion. Researchers have speculated that these hydrothermal effects should be common on Mars.[6] Ridges found in and around the center of Auki are evidence of hydrothermal processes. This crater contains ridges that may have been produced after fractures formed as a result of an impact. Using instruments on the Mars Reconnaissance Orbiter they found the minerals smectite (clay), silica, zeolite, serpentine, carbonate, and chlorite that are common in impact-induced hydrothermal systems on Earth.[7] [8] [9] [10] [11] [12] Evidence of other hydrothermal systems around craters other than Auki has been found by different groups of scientists.[13] [14] [15]

Close view of central portion of Auki, as seen by HiRISE Arrow indicates ridges. Sand dunes are present near the top of the image. Close view of central portion of Auki, as seen by HiRISE Arrow indicates ridges. Sand dunes are present near the top of the image.


Close view of ridges from previous image Arrow indicates an "X" shaped ridge. Close view of ridges from previous image Arrow indicates an "X" shaped ridge.

Channels

There is enormous evidence that water once flowed in river valleys and channels on Mars. Images of curved channels have been seen in images from Mars spacecraft dating back to the early 70's with the Mariner 9 orbiter.[16] [17] [18] [19] Vallis (plural valles) is the Latin word for 'valley. It is used in planetary geology for the naming of features on other planets, including what could be old river valleys that were discovered on Mars, when probes were first sent to Mars. The Viking Orbiters caused a revolution in our ideas about water on Mars; river valleys were found in many areas. Spacecraft cameras showed that floods of water broke through dams, carved deep valleys, eroded grooves into bedrock, and traveled thousands of kilometers.[20] [21] [22]

Linear ridge networks

Linear ridge networks are found in various places on Mars in and around craters.[23] 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. Scientists are not totally sure what caused these ridges, but one popular idea is that impacts created fractures in the surface, these fractures later acted as channels for fluids. Fluids hardened. With the passage of time, surrounding material was eroded away, thereby leaving hard ridges behind. Since the ridges occur in locations with clay, these formations could serve as a marker for past water because clay requires water to be produced.[24] [25] [26] Water here could have supported past life in these locations. Clay near these structures could preserve fossils or other traces of past life.

Dunes

Close, color view of dunes Ripples are visible on dune surface.

                          Close, color view of dunes  Ripples are visible on dune surface.

Sand dunes have been found in many places on Mars. They are usually in low spots—like crater floors. In HiRISE images they can appear in a variety of pretty colors. The colors are somewhat artificial. NASA modifies colors to determine mineral composition. The presence of dunes shows that the planet has an atmosphere with wind, for dunes require wind to pile up the sand. Although Mars has strong winds at times, we must remember that the Martian atmosphere is only about 1 % as dense as the Earth's. Hence, a wind speed of a 60-mph storm on Mars would feel more like 6 mph (9.6 km/hr).[27] Most dunes on Mars are black because of the weathering of the volcanic rock basalt.[28] [29] Black sand can be found on Earth on Hawaii and on some tropical South Pacific islands.[30] Sand is common on Mars due to the old age of the surface that has allowed rocks to erode into sand. Dunes on Mars have been observed to move many meters.[31] [32] [33] For a dune to move, sand moves up the windward side and then falls down the leeward side of the dune, thus caused the dune to go toward the leeward side (or slip face).[34] When iimages are enlarged, some dunes on Mars display ripples on their surfaces.[35]

Layers

Many places on Mars show rocks arranged in layers. Rock can form layers in a variety of ways. Volcanoes, wind, or water can produce layers.[36]

Layered features

                           Layered features


Columnar Jointing

Lava flows sometimes cool to form large groups of more-or-less equally sized columns.[37] [38] These joints have been seen on Mars.[39]


Close view of crater wall with columnar jointing labeled

  Close view of crater wall with columnar jointing labeled  

Other views in Mare Tyrrhenum quadrangle

Viking map of Mare Tyrrhenum quadrangle showing some major features. The small colored rectangles represent areas imaged in high resolution with camera on Mars Global Surveyor.

Viking map of Mare Tyrrhenum quadrangle showing some major features. The small colored rectangles represent areas imaged in high resolution with camera on Mars Global Surveyor.


Tyrrhenus Mons, as seen by HiRISE and suggested by Ehsan Sanaei's high school astronomy club in Yazd, Iran. it is great that NASA allows amateurs, especially kids to help explore Mars.


Tyrrhenus Mons, as seen by HiRISE and suggested by Ehsan Sanaei's high school astronomy club in Yazd, Iran. it is great that NASA allows amateurs, especially kids to help explore Mars.


Ejecta lobes indicated with arrows in a crater

                                             Ejecta lobes indicated with arrows in a crater

See also

References

Further reading

  • Lorenz, R. 2014. The Dune Whisperers. The Planetary Report: 34, 1, 8-14
  • Lorenz, R., J. Zimbelman. 2014. Dune Worlds: How Windblown Sand Shapes Planetary Landscapes. Springer Praxis Books / Geophysical Sciences.

External links

  • High resolution video by Seán Doran of overflight of part of north central Mare Tyrrhenum quadrangle, including Tinto Vallis and Amenthes Planum (continues across the equator into Amenthes quadrangle)
  • 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.
  • Hartmann, W. 2003. A Traveler's Guide to Mars. Workman Publishing. NY NY.
  • Carr, M. 2007. The surface of Mars. Cambridge University Press. New York.
  • http://www.lpi.usra.edu/publications/slidesets/stones/
  • http://www.indiana.edu/~sierra/papers/2003/Patterson.html.
  • Osinski, G., et al. 2013. Impact-generated hydrothermal systems on Earth and Mars. Icarus: 224, 347-363.
  • Carrozzo, F. et al. 2017. Geology and mineralogy of the Auki Crater, Tyrrhena Terra, Mars: A possible post impact-induced hydrothermal system. 281: 228-239
  • Loizeau, D. et al. 2012. Characterization of hydrated silicate-bearing outcrops in tyrrhena Terra, Mars: implications to the alteration history of Mars. Icarus: 219, 476-497.
  • Naumov, M. 2005. Principal features of impact-generated hydrothermal circulation systems: mineralogical and geochemical evidence. Geofluids: 5, 165-184.
  • Ehlmann, B., et al. 2011. Evidence for low-grade metamorphism, hydrothermal alteration, and diagenesis on Mars from phyllosilicate mineral assemblages. Clays Clay Miner: 59, 359-377.
  • Osinski, G. et al. 2013. Impact-generated hydrothermal systems on Earth and Mars. Icarus: 224, 347-363.
  • Schwenzer, S., D. Kring. 2013. Alteration minerals in impact-generated hydrothermal systems – Exploring host rock variability. Icarus: 226, 487-496.
  • Marzo, G., et al. 2010. Evidence for hesperian impact-induced hydrothermalism on Mars. Icarus: 667-683.
  • Mangold, N., et al. 2012. Hydrothermal alteration in a late hesperian impact crater on Mars. 43rd Lunar and Planetary Science. #1209.
  • Tornabene, L., et al. 2009. Parautochthonous megabreccias and possible evidence of impact-induced hydrothermal alteration in holden crater, Mars. 40th LPSC. #1766.
  • Baker, V. 1982. The Channels of Mars. Univ. of Tex. Press, Austin, TX
  • Baker, V., R. Strom, R., V. Gulick, J. Kargel, G. Komatsu, V. Kale. 1991. Ancient oceans, ice sheets and the hydrological cycle on Mars. Nature 352, 589–594.
  • Carr, M. 1979. Formation of Martian flood features by release of water from confined aquifers. J. Geophys. Res. 84, 2995–300.
  • Komar, P. 1979. Comparisons of the hydraulics of water flows in Martian outflow channels with flows of similar scale on Earth. Icarus 37, 156–181.
  • Kieffer|title=Mars|url=https://books.google.com/books?id=NoDvAAAAMAAJ%7Caccessdate=7 March 2011|date=1992|publisher=University of Arizona Press|
  • Raeburn, P. 1998. Uncovering the Secrets of the Red Planet Mars. National Geographic Society. Washington D.C.
  • Moore, P. et al. 1990. The Atlas of the Solar System. Mitchell Beazley Publishers NY, NY.
  • 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.
  • Mangold et al. 2007. Mineralogy of the Nili Fossae region with OMEGA/Mars Express data: 2. Aqueous alteration of the crust. J. Geophys. Res., 112, doi:10.1029/2006JE002835.
  • Mustard et al., 2007. Mineralogy of the Nili Fossae region with OMEGA/Mars Express data: 1. Ancient impact melt in the Isidis Basin and implications for the transition from the Noachian to Hesperian, J. Geophys. Res., 112.
  • Mustard et al., 2009. Composition, Morphology, and Stratigraphy of Noachian Crust around the Isidis Basin, J. Geophys. Res., 114, doi:10.1029/2009JE003349.
  • https://www.space.com/30663-the-martian-dust-storms-a-breeze.html
  • http://hirise.lpl.arizona.edu/ESP_016459_1830
  • Michael H. Carr|title=The surface of Mars|url=https://books.google.com/books?id=uLHlJ6sjohwC%7Caccessdate=21 March 2011|year=2006|publisher=Cambridge University Press|
  • https://www.desertusa.com/desert-activity/sand-dune-wind1.html
  • https://www.youtube.com/watch?v=ur_TeOs3S64
  • https://uanews.arizona.edu/story/the-flowing-sands-of-mars
  • Cardinale, M., S. Silvestro, D. Vazd, T. Michaels, M. Bourke, G. Komatsu, L. Marinangeli. 2016. Present-day aeolian activity in Herschel Crater, Mars. Icarus: 265, 139-148.
  • Namowitz, S., Stone, D. 1975. earth science the world we live in. American Book Company. New York.
  • https://www.jpl.nasa.gov/news/news.php?feature=6551
  • http://hirise.lpl.arizona.edu?PSP_008437_1750 |title=HiRISE | High Resolution Imaging Science Experiment |publisher=Hirise.lpl.arizona.edu?psp_008437_1750 |date= |
  • http://volcano.oregonstate.edu/columnar-jointing
  • Bates, R. and J. Jackson (eds.) 1976. Dictionary of Geological Terms. Doubleday, New York.
  • McEwen, A. et al. 2017. Mars The Pristine Beauty of the Red Planet. University of Arizona Press. Tucson.