Cryovolcanic rates on Ceres revealed by topography

  title={Cryovolcanic rates on Ceres revealed by topography},
  author={Michael M. Sori and Hanna G. Sizemore and Shane Byrne and Ali M. Bramson and Michael T. Bland and Nathaniel T. Stein and Christopher T. Russell},
  journal={Nature Astronomy},
Cryovolcanism, defined here as the extrusion of icy material from depth, may be an important planetary phenomenon in shaping the surfaces of many worlds in the outer Solar System and revealing their thermal histories1–3. However, the physics, chemistry and ubiquity of this geologic process remain poorly understood, especially in comparison to the better-studied silicate volcanism on the terrestrial planets. Ceres is the only plausibly cryovolcanic world to be orbited by a spacecraft up to now… Expand
Post-impact cryo-hydrologic formation of small mounds and hills in Ceres’s Occator crater
The intimate mixture of ice and silicate within the uppermost few kilometres of Ceres influences its geology and the evolution of its subsurface. Both ground ice and cryovolcanic processes have beenExpand
Dome formation on Ceres by solid-state flow analogous to terrestrial salt tectonics
The dwarf planet Ceres’s outer crust is a complex, heterogeneous mixture of ice, clathrates, salts and silicates. Numerous large domes on Ceres’s surface indicate a degree of geological activity.Expand
Thermal convection in the crust of the dwarf planet – I. Ceres
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Slurry extrusion on Ceres from a convective mud-bearing mantle
Ceres is a 940-km-diameter dwarf planet that is predominantly composed of silicates and water ice. In Ceres’ partially differentiated interior, extrusive processes have led to the emplacement on itsExpand
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Evidence of non-uniform crust of Ceres from Dawn’s high-resolution gravity data
The gravity and shape data acquired by the Dawn spacecraft during its primary mission revealed that Ceres is partially differentiated with an interior structure consistent with a volatile-rich crust,Expand
Fresh emplacement of hydrated sodium chloride on Ceres from ascending salty fluids
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Ceres: Astrobiological Target and Possible Ocean World.
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Islands of ice on Mars and Pluto
Ice sheets, such as the polar layered deposits (PLDs) of Mars, are of great interest as records of past climate. Smaller outlier ice deposits near the north and south PLDs are likely more sensitiveExpand
Relict Ocean Worlds: Ceres
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Cryovolcanism on Ceres
It is proposed that hydrated salts with low eutectic temperatures and low thermal conductivities enabled the presence of cryomagmatic liquids within Ceres, a key process for Ceres’ evolution as recorded by the aqueously altered, secondary minerals observed on the surface. Expand
Volcanism on Mars
More than 15 years of planetary exploration of Mars have given insight into the geologic processes that have shaped its surface. The newly acquired Viking data have shown that volcanism is one of theExpand
The vanishing cryovolcanoes of Ceres
Ahuna Mons is a 4-km-tall mountain on Ceres interpreted as a geologically young cryovolcanic dome. Other possible cryovolcanic features are more ambiguous, implying that cryovolcanism is only aExpand
The interior structure of Ceres as revealed by surface topography
Abstract Ceres, the largest body in the asteroid belt (940 km diameter), provides a unique opportunity to study the interior structure of a volatile-rich dwarf planet. Variations in a planetaryExpand
The geomorphology of Ceres
The global trend of lobate flows suggests that differences in their geomorphology could be explained by variations in ice content and temperature at the near surface, and the identification of these potentially ice-related features suggests that there may be more ice within localized regions of Ceres’ crust. Expand
A Possible Brine Reservoir Beneath Occator Crater: Thermal and Compositional Evolution and Formation of the Cerealia Dome and Vinalia Faculae
Abstract The Dawn spacecraft has imaged several putative cryovolcanic features on Ceres, and several lines of evidence point to past cryovolcanic activity at Occator crater. It is therefore possibleExpand
The Crust of the Moon as Seen by GRAIL
The Moon's gravity field shows that the lunar crust is less dense and more porous than was thought, and high-resolution gravity data obtained from the dual Gravity Recovery and Interior Laboratory (GRAIL) spacecraft show that the bulk density of the Moon's highlands crust is substantially lower than generally assumed. Expand
The missing large impact craters on Ceres
The results indicate that a significant population of large craters has been obliterated, implying that long-wavelength topography viscously relaxed or that Ceres experienced protracted widespread resurfacing. Expand
Limits on modes of lithospheric heat transport on Venus from impact crater density
We present a formalism by which the size-frequency distribution of impact craters on Venus may be used to estimate upper bounds on the mean global rates of volcanic resurfacing and lithosphericExpand
Brine volcanism and the interior structures of asteroids and icy satellites
Abstract Cryovolcanism is among the foremost processes responsible for modifying the surfaces of icy satellites. Volcanic brine petrogenesis in ammonia-deficient satellites should mainly involveExpand