The central pit and dome at Cerealia Facula bright deposit and floor deposits in Occator crater, Ceres: Morphology, comparisons and formation

@article{Schenk2019TheCP,
  title={The central pit and dome at Cerealia Facula bright deposit and floor deposits in Occator crater, Ceres: Morphology, comparisons and formation},
  author={Paul M. Schenk and Hanna G. Sizemore and Britney E. Schmidt and Julie C. Castillo‐Rogez and Maria Cristina De Sanctis and Timothy J. Bowling and Jennifer E. C. Scully and Debra L. Buczkowski and Lynnae C. Quick and Frank Preusker and Ryan S. Park and Carol A. Raymond and Christopher Russell},
  journal={Icarus},
  year={2019}
}
Abstract The prominent bright deposit Cerealia Facula, Ceres, coincides with the central depression (or central pit) of the recently formed 92 km-wide complex crater Occator. The central pit is 9–10 km wide and up to 1 km deep and is partially filled with a 700 m-high 2 km-wide dome. The upper surface of the central dome is densely fractured but the flanks are not, indicating that uplift of the dome surface occurred after the bright deposit was emplaced, and primarily through uplift of the… Expand
Ceres’ Occator crater and its faculae explored through geologic mapping
Abstract Occator crater is one of the most recognizable features on Ceres because of its interior bright regions, which are called the Cerealia Facula and Vinalia Faculae. Here we use high-resolutionExpand
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
The varied sources of faculae-forming brines in Ceres’ Occator crater emplaced via hydrothermal brine effusion
TLDR
It is reported that brine effusion emplaced the faculae in a brine-limited, impact-induced hydrothermal system of Occator crater of the dwarf planet Ceres, and that impact-derived fracturing enabled brines to reach the surface. Expand
Tectonic analysis of fracturing associated with occator crater
Abstract Occator crater, a Ceres crater that hosts multiple bright spots on its floor, has several sets of fractures associated with it. A tectonic analysis of each of these fracture sets suggestsExpand
Compositional control on impact crater formation on mid-sized planetary bodies: Dawn at Ceres and Vesta, Cassini at Saturn
Abstract High-resolution mapping of Ceres, Vesta and the icy satellites of Saturn, Uranus and Pluto reveals a rich variety of well-preserved impact crater morphologies on these low gravity bodies.Expand
Impact heat driven volatile redistribution at Occator crater on Ceres as a comparative planetary process
TLDR
Stereo imaging and topographic maps of Occator crater are shown revealing the influence of crustal composition on impact related melt and hydrothermal processes, and features to those on Mars, Earth and the Moon are compared. Expand
Topography and geology of Uranian mid-sized icy satellites in comparison with Saturnian and Plutonian satellites
Newly processed global imaging and topographic mapping of Uranus's five major satellites reveal differences and similarities to mid-sized satellites at Saturn and Pluto. Three modes of internal heatExpand
Impact Craters on Pluto and Charon and Terrain Age Estimates
Pluto's terrains display a diversity of crater retention ages ranging from areas with no identifiable craters to heavily cratered terrains. This variation in crater densities is consistent withExpand
Impact Craters on Pluto and Charon and Terrain Age Estimates
Pluto’s terrains display a diversity of crater retention ages ranging from areas with no identifiable craters to heavily cratered terrains. This variation in crater densities is consistent withExpand
A Global Inventory of Ice‐Related Morphological Features on Dwarf Planet Ceres: Implications for the Evolution and Current State of the Cryosphere
Examples of type 1 (A) and type 2 (B) landslides, fluidized or lobate ejecta (C), pitted materials (D), circumferential fractures (E), crater floor fractures (F), large domes (G), and small moundsExpand
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