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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).
Impact craters on Ceres exhibit a wide range of appearances. A large number of Cererian craters have central peaks. A large number of Cererian craters have central peaks. By correlating the presence or absence of central peaks with the sizes of the craters, scientists can infer the properties of Ceres's crust, such as how strong it is.
Venusian craters range from 3 kilometres (2 mi) to 280 kilometres (174 mi) in diameter. There are no craters smaller than 3 km, because of the effects of the dense atmosphere on incoming objects. Objects with less than a certain kinetic energy are slowed down so much by the atmosphere that they do not create an impact crater. [17]
As the trend in the Earth Impact Database for about 26 confirmed craters younger than a million years old shows that almost all are less than two km (1.2 mi) in diameter (except the three km (1.9 mi) Agoudal and four km (2.5 mi) Rio Cuarto), the suggestion that two large craters, Mahuika (20 km (12 mi)) and Burckle (30 km (19 mi)), formed only ...
The impactors that generated these events are thought to have been much larger than those that created the largest known still existing craters/impact structures on Earth, with the impactors having estimated diameters of ~20–50 kilometres (12–31 mi), with the craters generated by these impacts having an estimated diameter of 400–1,000 ...
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 ...
The rubble would have traveled at up to about 2,200 miles (3,600 km) per hour, they found. One of the canyons, called Vallis Planck, measures about 174 miles (280 km) long and 2.2 miles (3.5 km) deep.
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.