{{short description|Martian volcano}} {{Infobox feature on celestial object |name = Ceraunius Tholus |image = [[File:Ceraunius & Uranius tholi.jpg|240px]] |caption = ''[[2001 Mars Odyssey]]'' [[Thermal Emission Imaging System|THEMIS]] mosaic of '''Ceraunius Tholus''' (lower volcano) and [[Uranius Tholus]] (upper volcano). |type = mountain |coordinates = {{coord|24.25|N|262.75|E|globe:mars_type:landmark|display=inline,title}} |peak = ~{{convert|8500|m|ft|0}} }} '''Ceraunius Tholus''' is a volcano on [[Mars]] located in the [[Tharsis quadrangle]] at 24.25° north latitude and 262.75° east longitude,<ref>{{gpn|1106}}</ref> part of the [[Uranius group of volcanoes]]. It is {{convert|130|km|mi|0}} across, approximately {{convert|8500|m|ft|0}} high<ref name="Grego2012">{{cite book|author=Peter Grego|title=Mars and How to Observe It|url=https://archive.org/details/marshowtoobserve0000greg|url-access=registration|access-date=11 September 2019|date=1 June 2012|publisher=Springer|isbn=978-1-4614-2302-7|pages=[https://archive.org/details/marshowtoobserve0000greg/page/63 63]}}</ref> 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]].<ref>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</ref> 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.<ref name="Carr2006">{{cite book|author=Michael H. Carr|title=The surface of Mars|url=https://books.google.com/books?id=uLHlJ6sjohwC|access-date=21 March 2011|year=2006|publisher=[[Cambridge University Press]]|isbn=978-0-521-87201-0}}</ref><ref>{{cite journal | last1 = Gulick | first1 = Virginia C. | last2 = Baker | first2 = Victor R. | doi = 10.1029/JB095iB09p14325 | title = Origin and Evolution of Valleys on Martian Volcanoes | journal = Journal of Geophysical Research | year = 1990 | volume = 95 | pages= 14325–14344 | bibcode = 1990JGR....9514325G }}</ref> Interesting features on Ceraunius Tholus are three large canyons at the northwest flank of Ceraunius Tholus which are up to 2.5&nbsp;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 (crater)|Rahe]] (an oblique impact crater with measures of 35 × 18&nbsp;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.<ref>{{cite journal | last1=Fassett | first1=C | last2=Headiii | first2=J | title=Valley formation on martian volcanoes in the Hesperian: Evidence for melting of summit snowpack, caldera lake formation, drainage and erosion on Ceraunius Tholus | url=https://www.planetary.brown.edu/pdfs/3408.pdf | journal=Icarus | volume=189 | pages=118–135 | year=2007 | issue=1 | doi=10.1016/j.icarus.2006.12.021 | bibcode=2007Icar..189..118F | access-date=2009-03-14 | archive-date=2016-10-22 | archive-url=https://web.archive.org/web/20161022145617/http://www.planetary.brown.edu/pdfs/3408.pdf | url-status=dead }}</ref>

Ceraunius appears small compared to other larger volcanoes, but it is almost as tall as Earth's [[Mount Everest]].<ref>Morton, O. 2002. Mapping Mars. Picador, NY</ref>

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 (crater)|Paros]] lies south of Ceraunius Tholus, and the elongate crater [[Rahe (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.<ref>{{Cite journal |last=Forget |first=F. |last2=Haberle |first2=R.M. |last3=Montmessin |first3=F. |last4=Levrard |first4=B. |last5=Head |first5=J.W. |date=Jan 2006 |title=Formation of Glaciers on Mars by Atmospheric Precipitation at High Obliquity |url=https://doi.org/10.1126/science.1120335 |journal=Science |volume=311 |issue=5759 |pages=368-371}}</ref> A study analysing data gathered over Ceraunius Tholus by the [[Mars Orbiter Laser Altimeter]] concluded that there was likely to have been a period of significant snow and ice accumulation, and that snowmelt may have contributed to valley formation on Ceraunius Tholus, as well as the formation of a caldera lake.<ref>{{Cite journal |last=Fassett |first=Caleb I. |last2=Head III |first2=James W. |date=July 2007 |title=Valley formation on martian volcanoes in the Hesperian: Evidence for melting of summit snowpack, caldera lake formation, drainage and erosion on Ceraunius Tholus |url=https://doi.org/10.1016/j.icarus.2006.12.021 |journal=Icarus |volume=189 |issue=1 |pages=118-135 |via=Science Direct}}</ref> A subsequent study utilising high-resolution colour imagery from the Colour and Stereo Surface Imaging System onboard the [[European Space Agency|ESA]] [[Trace Gas Orbiter]] found evidence of periodic frost formation on Ceraunius Tholus.<ref>{{Cite journal |last=Valantinas |first=A. |last2=Thomas |first2=N. |display-authors=1 |date=June 2024 |title=Evidence for transient morning water frost deposits on the Tharsis volcanoes of Mars |url=https://doi.org/10.1038/s41561-024-01457-7 |journal=Nature Geoscience |issue=17 |pages=608-616}}</ref>

== Environment around Ceraunius Tholus == Ceraunius Tholus is on the Tharsis rise, also called the Tharsis bulge.<ref name="Carr2006"/> Tharsis is a land of great [[volcanoes]]. [[Olympus Mons]] is the tallest known volcano. [[Ascraeus Mons]] and [[Pavonis Mons]] are at least 320&nbsp;km across and are over 10&nbsp;km above the [[plateau]] that they sit on. The plateau is five to four seven kilometers above the zero altitude of Mars.<ref>Norton, O. 2002. Mapping Mars. Picador, New York.</ref> [[File:Tharsis Quadrangle map-la.svg|thumb|Map of Tharsis quadrangle with major features indicated. Tharsis contains many volcanoes, including Olympus Mons, the tallest known volcano in the [[Solar System]].]] <gallery> Image:Ceraunius Tholus Channel.JPG|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.

Image:Cerauniustholus.jpg|View of Ceraunius Tholus and Uranius Tholus from the [[Mars Orbiter Camera]] of ''[[Mars Global Surveyor]]''.

Image:Ceraunius Tholus 3D THEMIS dayIR-MOLA 5x vert.jpg|Computer-generated 3D view of Ceraunius Tholus with 5x vertical exaggeration. The image was obtained from THEMIS coverage plus [[Mars Orbiter Laser Altimeter|MOLA]] altimetry. The crater [[Rahe (crater)|Rahe]] is at left. </gallery> {{commons category|Ceraunius Tholus}}

==References== {{reflist}}

==See also== * [[Geography of Mars]] * [[Geology of Mars]] * [[Glaciers on Mars]] * [[HiRISE]] * [[List of mountains on Mars by height]] * [[Volcanoes on Mars]] * [[Volcanology of Mars]]

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[[Category:Volcanoes of Mars]] [[Category:Tharsis quadrangle]] [[Category:Shield volcanoes]]