Cryovolcanism on the icy satellites

@article{Kargel1994CryovolcanismOT,
  title={Cryovolcanism on the icy satellites},
  author={Jeffrey S. Kargel},
  journal={Earth, Moon, and Planets},
  year={1994},
  volume={67},
  pages={101-113}
}
  • J. Kargel
  • Published 1994
  • Geology
  • Earth, Moon, and Planets
Evidence of past cryovolcanism is widespread and extremely varied on the icy satellites. Some cryovolcanic landscapes, notably on Triton, are similar to many silicate volcanic terrains, including what appear to be volcanic rifts, calderas and solidified lava lakes, flow fields, breached cinder cones or stratovolcanoes, viscous lava domes, and sinuous rilles. Most other satellites have terrains that are different in the important respect that no obvious volcanoes are present. The preserved… 

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References

SHOWING 1-10 OF 32 REFERENCES

Volcanism and igneous processes in small icy satellites

The small saturnian satellites exhibit a remarkable diversity of surficial features1–3 including many which appear to be a consequence of internal activity: ‘wispy’ terrain, linear troughs, and

Ammonia-water volcanism on icy satellites: Phase relations at 1 atmosphere

Geology of the Uranian satellites

A geological analysis of six of the Uranus satellites observed in detail by Voyager 2 is presented. All of the satellites except the smallest, Puck, show evidence of cryovolcanic resurfacing: global

Fluid volcanism on Miranda and Ariel: Flow morphology and composition

Several types of volcanic units have been recognized on the icy Uranian satellites Miranda and Ariel. On Miranda, ridges characterized by crest grooves are up to 10 km wide and 500 m high. A

The evolution of Enceladus

Saturn's icy satellites - Thermal and structural models

The geology of Europa

The map units and lineations of Europa are detailed, and the geologic processes, and history, and thick and thin ice models of the satellite are discussed. It is concluded that Europa lacks evidence

Solid-State Ice Volcanism on the Satellites of Uranus

TLDR
These images provide the first observational evidence for solid-state ice volcanism in the solar system, and the initial viscosity of the flow material is found to have been no more than about 1016 poise, far lower than expected for H2O ice at the ambient surface temperatures in the uranian system.