 2001 Mars OdysseyTHEMIS mosaic ofCeraunius Tholus (lower volcano) andUranius Tholus (upper volcano). | |
| Feature type | mountain |
|---|---|
| Coordinates | 24°15′N262°45′E / 24.25°N 262.75°E /24.25; 262.75 |
| Peak | ~8,500 metres (27,887 ft) |
Ceraunius Tholus is a volcano onMars located in theTharsis quadrangle at 24.25° north latitude and 262.75° east longitude,[1] part of theUranius group of volcanoes. It is 130 kilometres (81 mi) across, approximately 8,500 metres (27,887 ft) high[2] and is named after a classicalalbedo 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 astratovolcano.[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 thecaldera 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 craterRahe (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'sMount 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 lateHesperian in age.
The craterParos lies south of Ceraunius Tholus, and the elongate craterRahe is to the north.
Some scientists believe thatglaciers may have existed on many of the volcanoes inTharsis including Olympus Mons, Ascraeus Mons, and Pavonis Mons.[8] A study analysing data gathered over Ceraunius Tholus by theMars 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.[9] A subsequent study utilising high-resolution colour imagery from the Colour and Stereo Surface Imaging System onboard theESATrace Gas Orbiter found evidence of periodic frost formation on Ceraunius Tholus.[10]
Ceraunius Tholus is on the Tharsis rise, also called the Tharsis bulge.[4] Tharsis is a land of greatvolcanoes.Olympus Mons is the tallest known volcano.Ascraeus Mons andPavonis Mons are at least 320 km across and are over 10 km above theplateau that they sit on. The plateau is five to four seven kilometers above the zero altitude of Mars.[11]
