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  2. Geology of Ceres - Wikipedia

    en.wikipedia.org/wiki/Geology_of_Ceres

    Ceres' shape is controlled mainly by gravity and spin, with only a 3% departure from hydrostatic equilibrium. Its best-fit shape is a triaxial ellipsoid with dimensions a = 483.1 km, b = 481.0, km and c = 445.9 km, with c being the north-south axis and a and b the semimajor and semiminor equatorial axes.

  3. List of geological features on Ceres - Wikipedia

    en.wikipedia.org/wiki/List_of_geological...

    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).

  4. Ceres (dwarf planet) - Wikipedia

    en.wikipedia.org/wiki/Ceres_(dwarf_planet)

    The active geology of Ceres is driven by ice and brines. Water leached from rock is estimated to possess a salinity of around 5%. Altogether, Ceres is approximately 50% water by volume (compared to 0.1% for Earth) and 73% rock by mass. [14] Ceres's largest craters are several kilometres deep, inconsistent with an ice-rich shallow subsurface.

  5. Dwarf planet Ceres is 'ocean world' with salty water deep ...

    www.aol.com/news/dwarf-planet-ceres-ocean-world...

    Ceres, the largest object in the asteroid belt between Mars and Jupiter, is an "ocean world" with a big reservoir of salty water under its frigid surface, scientists said in findings that raise ...

  6. Geology of solar terrestrial planets - Wikipedia

    en.wikipedia.org/wiki/Geology_of_solar...

    The geology of the dwarf planet, Ceres, was largely unknown until Dawn spacecraft explored it in early 2015. However, certain surface features such as "Piazzi", named after the dwarf planets' discoverer, had been resolved.[a] Ceres's oblateness is consistent with a differentiated body, a rocky core overlain with an icy mantle.

  7. File:Interior Structure of Ceres - diagram.svg - Wikipedia

    en.wikipedia.org/wiki/File:Interior_Structure_of...

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  8. Water on terrestrial planets of the Solar System - Wikipedia

    en.wikipedia.org/wiki/Water_on_terrestrial...

    The current Venusian atmosphere has only ~200 mg/kg H 2 O(g) in its atmosphere and the pressure and temperature regime makes water unstable on its surface. Nevertheless, assuming that early Venus's H 2 O had a ratio between deuterium (heavy hydrogen, 2H) and hydrogen (1H) similar to Earth's Vienna Standard Mean Ocean Water of 1.6×10 −4, [7] the current D/H ratio in the Venusian atmosphere ...

  9. Occator (crater) - Wikipedia

    en.wikipedia.org/wiki/Occator_(crater)

    [4] [5] In August 2020, NASA confirmed that Ceres was a water-rich body with a deep reservoir of brine that percolated to the surface in various locations causing the "bright spots", including those in Occator crater. [6] [7] The percolation of brine from a deep internal reservoir to the surface at Occator crater was first modeled in 2019. [8]