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Ceraunius Tholus

Ceraunius Tholus
2001 Mars Odyssey THEMIS mosaic of Ceraunius Tholus (lower volcano) and Uranius Tholus (upper volcano).
Feature typemountain
Coordinates24°15′N 262°45′E / 24.25°N 262.75°E / 24.25; 262.75
Peak~8,500 metres (27,887 ft)

Ceraunius Tholus is a volcano on Mars located in the Tharsis quadrangle at 24.25° north latitude and 262.75° east longitude,[1] part of the Uranius group of volcanoes. It is 130 kilometres (81 mi) across, approximately 8,500 metres (27,887 ft) high[2] and is named after a classical albedo feature name.

It is generally believed to be a basaltic shield with the lower part buried beneath plain forming lavas. Earlier interpretations suggested that it is a stratovolcano.[3] The slopes on Ceraunius Tholus are quite steep with an average slope of 8° with many radial erosion channels and pitted valleys extending from just below the rim of the caldera toward the base of the volcano. The current view is that the valleys were eroded by water.[4][5] Interesting features on Ceraunius Tholus are three large canyons at the northwest flank of Ceraunius Tholus which are up to 2.5 km wide and 300 m deep. The biggest of these three also appears to be the youngest and protrude from the lowest point of the volcanic caldera and ends at the interesting crater Rahe (an oblique impact crater with measures of 35 × 18 km), just north from the volcano where it formed a depositional fan. Its origin is still debatable and there are four main models proposed: fluvial action, volcanic flows, valley being a lava channel or some combination of previously mentioned models.[6]

Ceraunius appears small compared to other larger volcanoes, but it is almost as tall as Earth's Mount Everest.[7]

The caldera of Ceranius Tholus is also dotted with many collapse pits, which are distinct from impact craters as they have no rim and vary in abundance across the caldera. Ceraunius Tholus is probably late Hesperian in age.

The crater Paros lies south of Ceraunius Tholus, and the elongate crater Rahe is to the north.

Glaciers

Some scientists believe that glaciers may have existed on many of the volcanoes in Tharsis including Olympus Mons, Ascraeus Mons, and Pavonis Mons.[8] Ceraunius Tholus may have even had its glaciers melt to form some temporary lakes in the past. The smoothness and flatness of the Ceraunius Tholus caldera floor suggests that in the past meltwater accumulated in a caldera lake.[9][10]

Environment around Ceraunius Tholus

Ceraunius Tholus is on the Tharsis rise, also called the Tharsis bulge.[4] Tharsis is a land of great volcanoes. Olympus Mons is the tallest known volcano. Ascraeus Mons and Pavonis Mons are at least 320 km across and are over 10 km above the plateau that they sit on. The plateau is five to four seven kilometers above the zero altitude of Mars.[11]

Map of Tharsis quadrangle with major features indicated. Tharsis contains many volcanoes, including Olympus Mons, the tallest known volcano in the Solar System.
  • Ceraunius Tholus Channel, as seen by HiRISE. The summit crater of Ceraunius Tholus is just to the right of this picture. Click on image to see dark slope streaks. The scale bar is 1000 meters long.
    Ceraunius Tholus Channel, as seen by HiRISE. The summit crater of Ceraunius Tholus is just to the right of this picture. Click on image to see dark slope streaks. The scale bar is 1000 meters long.
  • View of Ceraunius Tholus and Uranius Tholus from the Mars Orbiter Camera of Mars Global Surveyor.
    View of Ceraunius Tholus and Uranius Tholus from the Mars Orbiter Camera of Mars Global Surveyor.
  • Computer-generated 3D view of Ceraunius Tholus with 5x vertical exaggeration. The image was obtained from THEMIS coverage plus MOLA altimetry. The crater Rahe is at left.
    Computer-generated 3D view of Ceraunius Tholus with 5x vertical exaggeration. The image was obtained from THEMIS coverage plus MOLA altimetry. The crater Rahe is at left.
Wikimedia Commons has media related to Ceraunius Tholus.

References

  1. ^ "Ceraunius Tholus". Gazetteer of Planetary Nomenclature. USGS Astrogeology Research Program.
  2. ^ Peter Grego (1 June 2012). Mars and How to Observe It. Springer. pp. 63. ISBN 978-1-4614-2302-7. Retrieved 11 September 2019.
  3. ^ Characteristics of valleys on Ceraunius Tholus and their formation: Part I. Caleb I. Fassett and James W. Head, Dept. of Geological Sciences, Brown University, Providence, RI 02912. Microsymposium 38, MS016, 2003
  4. ^ a b Michael H. Carr (2006). The surface of Mars. Cambridge University Press. ISBN 978-0-521-87201-0. Retrieved 21 March 2011.
  5. ^ Gulick, Virginia C.; Baker, Victor R. (1990). "Origin and Evolution of Valleys on Martian Volcanoes". Journal of Geophysical Research. 95: 14325–14344. Bibcode:1990JGR....9514325G. doi:10.1029/JB095iB09p14325.
  6. ^ Fassett, C; Headiii, J (2007). "Valley formation on martian volcanoes in the Hesperian: Evidence for melting of summit snowpack, caldera lake formation, drainage and erosion on Ceraunius Tholus" (PDF). Icarus. 189 (1): 118–135. Bibcode:2007Icar..189..118F. doi:10.1016/j.icarus.2006.12.021. Archived from the original (PDF) on 2016-10-22. Retrieved 2009-03-14.
  7. ^ Morton, O. 2002. Mapping Mars. Picador, NY
  8. ^ http://www.lpi.edu/meetings/polar2003/pdf/8105.pdf[permanent dead link‍]
  9. ^ http://www.planetary.brown.edu/pdfs/3408.pdf Archived 2016-10-22 at the Wayback Machine [bare URL PDF]
  10. ^ http://www.mars.asu/christensen/advancedmarsclass/shean_glaciers_2005.pdf[permanent dead link‍]
  11. ^ Norton, O. 2002. Mapping Mars. Picador, New York.

See also
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