Cryovolcanism on the icy satellites

Abstract

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 record of cryovolcanism generally is believed to have formed by eruptions of aqueous solutions and slurries. Even Triton's volcanic crust, which is covered by nitrogen-rich frost, is probably dominated by water ice. Nonpolar and weakly polar molecular liquids (mainly N2, CH4, CO, CO2, and Ar), may originate by decomposition of gas-clathrate hydrates and may have been erupted on some icy satellites, but without water these substances do not form rigid solids that are stable against sublimation or melting over geologic time. Triton's plumes, active at the time of Voyager 2's flyby, may consist of multicomponent nonpolar gas mixtures. The plumes may be volcanogenic fumaroles or geyserlike emissions powered by deep internal heating, and, thus, the plumes may be indicating an interior that is still cryomagmatically active; or Triton's plumes may be powered by solar heating of translucent ices very near the surface. The Uranian and Neptunian satellites Miranda, Ariel, and Triton have flow deposits that are hundreds to thousands of meters thick (implying highly viscous lavas); by contrast, the Jovian and Saturnian satellites generally have plains-forming deposits composed of relatively thin flows whose thicknesses have not been resolved in Voyager images (thus implying relatively low-viscosity lavas). One possible explanation for this inferred rheological distinction involves a difference in volatile composition of the Uranian and Neptunian satellites on one hand and of the Jovian and Saturnian satellites on the other hand. Perhaps the Jovian and Saturnian satellites tend to have relatively "clean" compositions with water ice as the main volatile (ammonia and water-soluble salts may also be present). The Uranian and Neptunian satellites may possess large amounts of a chemically unequilibrated comet-like volatile assemblage, including methanol, formaldehyde, and a host of other highly water- and ammonia-water-soluble constituents and gas clathrate hydrates. These two volatile mixtures would produce melts that differ enormously in viscosity The geomorphologic similarity in the products of volcanism on Earth and Triton may arise partly from a rheological similarity of the ammonia-water-methanol series of liquids and the silicate series ranging from basalt to dacite. An abundance of gas clathrate hydrates hypothesized to be contained by the satellites of Uranus and Neptune could contribute to evidence of explosive volcanism on those objects.

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References

  1. Burns, J.A. (1986) Some background about satellites, in J.A. Burns and M.S. Matthews (eds.),Satellites, University of Arizona Press, Tucson, pp. 1–38.

    Google Scholar 

  2. Clark, R.N., Fanale, F.P., and Gaffey, M.J. (1986) Surface composition of natural satellites, in J.A. Burns and M.S. Matthews (eds.),Satellites, University of Arizona Press, Tucson, pp. 437–491.

    Google Scholar 

  3. Consolmagno, G.J., and Lewis, J.S. (1978) The evolution of satellite interiors and surfaces,Icarus 34, 280–293.

    Google Scholar 

  4. Croft, S.K. (1992), Proteus: Geology, shape, and catastrophic disruption,Icarus 99, 402–419.

    Google Scholar 

  5. Croft, S.K., and Soderblom, L.A. (1991) Geology of the Uranian satellites, in J.T. Bergstralh, E.D. Miner, and M.S. Matthews (eds.),Uranus, University of Arizona Press, Tucson, pp. 561–628.

    Google Scholar 

  6. Croft, S.K., Kargel, J.S., Kirk, R.L., Moore, J.M., Schenk, P.M., and Strom, R.G. (1995) The geology of Triton, in D.P. Cruikshank (ed.),Neptune and Triton, University of Arizona Press, Tucson (in press).

    Google Scholar 

  7. Cruikshank, D.P.,et al. (1991) Tentative identification of CO and CO2 ices on Triton,Bull. Amer. Astronom. Soc. 23, 1208.

    Google Scholar 

  8. Ellsworth, K., and G. Schubert (1983) Saturn's icy satellites: Thermal and structural models,Icarus 54, 490–510.

    Google Scholar 

  9. Farinella, P., Paolicchi, P., Strom, R.G., Kargel, J.S., and Zappalá, V. (1990) The fate of Hyperion's fragments,Icarus 83, 186–204.

    Google Scholar 

  10. Jankowski, D.G., and S.W. Squyres (1988) Solid-state ice volcanism on the satellites of Uranus,Science 241, 1322.

    Google Scholar 

  11. Johnson, T.V., R.H. Brown, and J.B. Pollack (1987) Uranus satellites: Densities and composition,J. Geophys. Res. 92, 14,884–14,894

    Google Scholar 

  12. Kargel, J.S., and R.G. Strom (1990) Cryovolcanism on Triton,Lunar Planet. Sci. Conf. XXI, 599–600.

    Google Scholar 

  13. Kargel, J.S., 1991, Brine volcanism and the interior structures of asteroids and icy satellites,Icarus 94, 368–390.

    Google Scholar 

  14. Kargel, J.S., S.K. Croft, J.I. Lunine, and J.S. Lewis (1991) Rheological properties of ammonia-water liquids and crystal-liquid slurries: Planetological applications,Icarus 89, 93–112.

    Google Scholar 

  15. Kargel, J.S. (1992) Ammonia-water volcanism on icy satellites: Phase relations at 1 atmosphere,Icarus 100, 556–574.

    Google Scholar 

  16. Kirk, R.L., Soderblom, L.A., Brown, R.H., Kieffer, S.W., and Kargel, J.K. (1995) Triton's plumes: Discovery, characteristics, and models, in D.P. Cruikshank (ed.),Neptune and Triton, The University of Arizona Press, Tucson (in press).

    Google Scholar 

  17. Lewis, J.S. (1971) Satellites of the outer planets: Their chemical and physical nature,Icarus 15, 174–185.

    Google Scholar 

  18. Lewis, J.S. (1972) Low-temperature condensation from the solar nebula,Icarus 16, 241–252.

    Google Scholar 

  19. Lucchitta, B.K., and Soderblom, L.A. (1982) The geology of Europa, in D. Morrison (ed.),Satellites of Jupiter, The University of Arizona Press, Tucson, pp. 521–555.

    Google Scholar 

  20. Prinn, R.G., and B. Fegley, Jr. (1988) Solar nebula chemistry: Origin of planetary, satellite, and cometary volatiles, in S.K. Atreya, J.B. Pollack, and M.S. Matthews (eds.),Planetary and Satellite Atmospheres: Origin and Evolution, University of Arizona Press, Tucson, pp. 78–136.

    Google Scholar 

  21. Rothery, D.A. (1992)Satellites of the Outer Planets: Worlds in Their Own Right, Oxford University Press, New York, pp. 208.

    Google Scholar 

  22. Schenk, P.M. (1990) Fluid volcanism on Ariel and Miranda: Flow morphology and composition,J. Geophys. Res. 96, 1887–1906.

    Google Scholar 

  23. Shoemaker, E.M., Lucchitta, B.K., Plescia, J.B., Squyres, S.W., and Wilhelms, D.E. (1982), The geology of Ganymede, in D. Morrison (ed.),Satellites of Jupiter, The University of Arizona Press, Tucson, pp. 435–520.

    Google Scholar 

  24. Smith, B.A.,et al. (1979) The Jupiter system through the eyes of Voyager 1,Science 204, 951–972.

    Google Scholar 

  25. Smith, B.A.,et al. (1982) A new look at the Saturn system: The Voyager 2 images,Science 215, 504–536.

    Google Scholar 

  26. Smith, B.A.,et al. (1986) Voyager 2 in the Uranian system: Imaging science results,Science 233, 43–64.

    Google Scholar 

  27. Smith, B.A.,et al. (1989) Voyager 2 at Neptune: Imaging science results,Science 246, 1422–1429.

    Google Scholar 

  28. Squyres, S.W., R.T. Reynolds, P.M. Cassen, and S.J. Peale (1983) The evolution of Enceladus,Icarus 53, 319–331.

    Google Scholar 

  29. Squyres, S.W., R.T. Reynolds, A.L. Summers, and F. Shung (1988) Accretional heating of the satellites of Saturn and Uranus,J. Geophys. Res. 93, 8779–8794.

    Google Scholar 

  30. Stevenson, D.J. (1982) Volcanism and igneous processes in small icy satellites,Nature 298, p. 142–144.

    Google Scholar 

  31. Strom, R.G. (1986) The solar system cratering record: Voyager 2 results at Uranus and implications for the origin of impacting objects,Icarus 70, 517–535.

    Google Scholar 

  32. Thomas, P.C. (1989) The shapes of small satellites,Icarus 77, 248–274.

    Google Scholar 

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Kargel, J.S. Cryovolcanism on the icy satellites. Earth Moon Planet 67, 101–113 (1994). https://doi.org/10.1007/BF00613296

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Keywords

  • Clathrate
  • Lava Dome
  • Lava Lake
  • Cinder Cone
  • Explosive Volcanism