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Interiors of icy bodies in the solar system (as of 2010)

Interiors of icy bodies in the solar system (as of 2010)

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Doug Ellison, Emily Lakdawalla, and Bob Pappalardo. Internal models based mostly on Hauke Hussmann, Frank Sohl, and Tilman Spohn, 2006, except for Titan (Giuseppi Mitri et al., 2010) and the Galilean moons (Bob Pappalardo, personal communication).

Interiors of icy bodies in the solar system (as of 2010)
Many bodies in our solar system may contain oceans. Jupiter's ice-coated moons (Europa, Ganymede, and Callisto) probably contain internal saltwater oceans. The more distant large and medium-sized icy moons, the icy dwarf planets, and tiny Enceladus may contain colder ammonia-water oceans. Oceans in icy satellites could be a common feature throughout the universe, while Earth's surface ocean may be the more unusual case. These interior models were developed by many geophysicists from data about the sizes, densities, and orbital characteristics of each body.

This work is licensed under a Creative Commons Attribution 3.0 Unported License. For uses not allowed by that license, contact us to request publication permission from the copyright holder: Bob Pappalardo : Doug Ellison : Emily Lakdawalla

Original image data dated on or about January 1, 2010

Explore related images: Enceladus, BMSIL, the solar system, Titan, Rhea, miscellaneous trans-Neptunian objects, Saturn's moons, Jupiter's moons, trans-neptunian objects, infographic, pretty pictures, Pluto, scale comparisons, Charon, 136199 Eris (2003 UB313), comparative planetology, Triton

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