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Dive into the captivating realm of moons and satellites in our solar system, from the volcanic activity on Io to the icy surfaces of Europa and the ancient terrains of Ganymede. Witness the unique features of each celestial body and ponder on the mysteries of their origins and geological processes. From the sulfuric compounds on Io to the potential liquid water beneath Europa's surface, each satellite holds its own secrets waiting to be unraveled. Embark on this cosmic odyssey and expand your understanding of the diverse worlds orbiting the planets.
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Satellites Chapter 14
Fig. 14.1 Tidal Heating of Io
Fig. 14.2 Orbital Resonance
Fig. 14.3 Phobos, Martian Satellite
Fig. 14.4 Phobos, Martian Satellite
Fig. 14.5 Deimos (Mars)
Fig. 14.6 Deimos, close up view
Fig. 14.7 Io Sulfur and sulfuric compounds Volcanic activity
Fig. 14.8 Plume on the Limb of Io
Fig. 14.10 Volcanic eruption on Io
Fig. 14.11 Two different images of Io 17 years apart (Voyager and Galileo)
Fig. 14.12 Model for the sufrace of Io
Fig. 14.13 Europa (from Galileo) Smooth, highly reflective surface crisscrossed by dark lines. Water ice. Liquid water underneath? Evidence of tidal forces from Jupiter.
Fig. 14.14 Europa’s Interior Structure
Fig. 14.15 Europa
Fig. 14.16 Ice Rafts on Europa
Fig. 14.18 Ganymede Ancient dark terrain separated By light-colored terrain
Fig. 14.19 Faulting on Ganymede
Fig. 14.20 A view across Ganymede
Fig. 14.21 Callisto
Fig. 14.22 Callisto
Fig. 14.23 A scarp on Callisto
Fig. 14.25 Rhea (1530 km)
Fig. 14.28 Tethys, (1050 km)
Fig. 14.29 Iapetus (1440 km)
Fig. 14.30 Enceladus (500 km)
Fig. 14.31 Icy material from Enceladus
Fig. 14.32 Titan (5150 km)
Fig. 14.33 Panoramic view of Titan
Fig. 14.34 At the surface of Titan (From Huygens)
Fig. 14.36 Umbriel (Uranus)
Fig. 14.37 Oberon (Uranus)
Fig. 14.38 Titania (Uranus)
Fig. 14.39 Ariel (Uranus)
Fig. 14.40 Miranda, Uranus)
Fig. 14.41 Coronae on Miranda (Uranus)
Fig. 14.45 Triton
Fig. 14.46 Triton
