Artwork Image Gallery
The KISS images below are public domain, but must be accompanied by the appropriate image credit.
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A schematic diagram of tidal deformation for a tidally-locked satellite orbiting a planet. Tides deform the satellite at all distances, although deformation is strongest when the satellite is closest to the planet (pericenter) and weakest when the satellite is furthest from the planet (apocenter). B–E, Schematic diagrams of how tides affect the orbit of a tidally-locked satellite (based on Burns and Matthews, 1986). -
Schematic of the Jovian and Saturnian systems. The top panels show the orbital architecture of the system, with the host planet and orbits to scale. Relevant mean-motion resonances are identified in red. The bottom panels show the satellites to scale with one another. We focus on the major satellites. Listed physical parameters include the diameter (d), bulk density (ρ), and rotational period (P)—which for all of the satellites is equal to their orbital period, as they are all tidally locked with their host planet. Schematic of the Jovian and Saturnian systems. The top panels show the orbital architecture of the system, with the host planet and orbits to scale. Relevant mean-motion resonances are identified in red. The bottom panels show the satellites to scale with one another. We focus on the major satellites. Listed physical parameters include the diameter (d), bulk density (ρ), and rotational period (P)—which for all of the satellites is equal to their orbital period, as they are all tidally locked with their host planet.
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Cover artwork from the Tidal Heating – Lessons from Io and the Jovian System report. Io and the Jupiter system is a vibrant destination for exploration, and holds the keys to fundamental understanding of tidal heating across the cosmos. Artwork is color pencil on paper. Cover artwork from the Tidal Heating – Lessons from Io and the Jovian System report. Io and the Jupiter system is a vibrant destination for exploration, and holds the keys to fundamental understanding of tidal heating across the cosmos. Artwork is color pencil on paper.
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Schematic illustration of the solar system’s ocean worlds. All worlds are shown to scale with one another, although the size of the interior layers are only approximate. Schematic illustration of the solar system’s ocean worlds. All worlds are shown to scale with one another, although the size of the interior layers are only approximate.
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Schematic illustration of the possible physical configurations of melt within Io and other partially molten silicate worlds. The scale of each block is of-order one centimeter. Schematic illustration of the possible physical configurations of melt within Io and other partially molten silicate worlds. The scale of each block is of-order one centimeter.
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Schematic illustration of the principles behind electromagnetic sounding of Io’s interior. Io experiences a time-varying external magnetic field (A), which produces eddy currents in Io’s conductive layers (B), which drives an induced magnetic field (C). The observed magnetic field around Io is a combination of these processes (D). The magnitude of the induced magnetic field is a function of the physical and electromagnetic properties of Io’s interior (E–G). Schematic illustration of the principles behind electromagnetic sounding of Io’s interior. Io experiences a time-varying external magnetic field (A), which produces eddy currents in Io’s conductive layers (B), which drives an induced magnetic field (C). The observed magnetic field around Io is a combination of these processes (D). The magnitude of the induced magnetic field is a function of the physical and electromagnetic properties of Io’s interior (E–G).
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Schematic illustration of the structure of Io’s interior, with arbitrary layer thicknesses, considering deep- (top) and shallow-mantle (bottom) end-member tidal dissipation scenarios within a solid interior (left panels) versus how dissipation processes would be affected by either a magma ocean, or globally extensive high-partial melt layer (i.e., a magmatic sponge; right panels). Schematic illustration of the structure of Io’s interior, with arbitrary layer thicknesses, considering deep- (top) and shallow-mantle (bottom) end-member tidal dissipation scenarios within a solid interior (left panels) versus how dissipation processes would be affected by either a magma ocean, or globally extensive high-partial melt layer (i.e., a magmatic sponge; right panels).
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The Jupiter system provides exciting destinations for groundbreaking new science, enabled by a variety of different spacecraft architectures, instruments, observations, and experiments. The Jupiter system provides exciting destinations for groundbreaking new science, enabled by a variety of different spacecraft architectures, instruments, observations, and experiments.
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