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Ceres has an axial tilt of 4°, [10] small enough for its polar regions to contain permanently shadowed craters that are expected to act as cold traps and accumulate water ice over time, similar to what occurs on the Moon and Mercury. About 0.14% of water molecules released from the surface are expected to end up in the traps, hopping an ...
Ceres is saturated with impact craters.Many have a central pit or bright spot. In the first batch of 17 names approved by the IAU, craters north of 20° north latitude had names beginning with A–G (with Asari being the furthest north), those between 20° north and south latitude beginning with H–R, and those further south beginning with S–Z (with Zadeni being the furthest south).
Ceres has spectral similarities to C-type asteroids, [3] which are rich in volatiles and carbonaceous compounds. Ceres is also sometimes classified as a G-type asteroid, [11] [12] which is a subtype of the Tholen C-class and characterized by abundant phyllosilicates, such as clay minerals. Ceres is not associated with any asteroid family or ...
As with many craters on Ceres, Haulani has been extensively modified by mass wasting processes, with landslide deposits from the crater rim covering parts of its floor. It is one of the youngest large craters on Ceres, estimated to have been formed between 1.7 and 5.9 million years ago. As a result, it is one of Ceres's brightest surface features.
The Kaali impacts (c. 1500 BC) during the Nordic Bronze Age may have influenced Estonian and Finnish mythology, [5] the Campo del Cielo (c. 2500 BC) could be in the legends of some Native Argentine tribes, [6] [7] while Henbury (c. 2700 BC) has figured in Australian Aboriginal oral traditions. [8] Macha crater field map One of the Kaali craters
Scientists have detected ice on the planet's surface, which could mean Ceres is hiding an ocean below its frozen crust. Dwarf planet Ceres may have a huge ocean that could support life Skip to ...
Of the world’s roughly 200 impact craters, 31 are located in Canada. Quebec itself has 10 other known impact sites. In the presentation to the Meteoritical Society, Rochette showed how the ring ...
Like most 70-150 km wide Ceresian impact craters, Occator has a central depression rather than a central peak, with its original central peak having collapsed into 9–10 km wide depression, ~1 km deeper than the crater floor. [17] [16] Data indicates that magnesium sulfide (MgS) deposits were in place after the central peak's uplift and collapse.