Satellites Chapter 14

Opener

Fig. 14.1 Tidal Heating of Io

Fig. 14.2 Orbital Resonance

Tab. 14.1

Fig. 14.3 Phobos, Martian Satellite

Phobos, Martian Satellite Fig. 14.4 Phobos, Martian Satellite

Fig. 14.5 Deimos (Mars)

Fig. 14.6 Deimos, close up view

Tab. 14.2

Sulfur and sulfuric compounds Fig. 14.7 Io Sulfur and sulfuric compounds Volcanic activity

Fig. 14.8 Plume on the Limb of Io

Fig. 14.9

Volcanic eruption on Io Fig. 14.10 Volcanic eruption on Io

Two different images of Io 17 years apart (Voyager and Galileo) Fig. 14.11 Two different images of Io 17 years apart (Voyager and Galileo)

Model for the sufrace of Io Fig. 14.12 Model for the sufrace of Io

Europa (from Galileo) Smooth, highly reflective surface 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.

Europa’s Interior Structure Fig. 14.14 Europa’s Interior Structure

Fig. 14.15 Europa

Fig. 14.16 Ice Rafts on Europa

Fig. 14.17

Ganymede Ancient dark terrain separated By light-colored terrain 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)

Icy material from Enceladus Fig. 14.31 Icy material from Enceladus

Fig. 14.32 Titan (5150 km)

Panoramic view of Titan 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. 14.43

Fig. 14.44

Fig. 14.45 Triton

Fig. 14.46 Triton

Fig. 14.47 Plumes on Triton