2500-15-large satellites

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Geology of Callisto • Close-up Look at an Area Near the Equator of Callisto • The Craters Have a Subdued Topography Relative to Those on the Rocky Terrestrial Planets • Subdued Look Due to Plastic Deformation of Ice – Unable to Retain Sharp Contours • No Big Basins – Instead, Bulls-Eye Pattern Is All That Remains Approximately 200 km Wide 300 km Long (The Size of Connecticut)
• High-Resolution View of the Surface of Callisto Taken by the Galileo Cameras in 1996 Geology of Callisto • The Surface Has Been Extensively Modified by Sublimation and Degradation of the Dirty-Ice Surface • Ice-Capped Peaks Appear Amid Smoother Plains of Darker Material Left Over When the Ice Evaporated
Page 1 and 2: Worlds of Fire and Ice: The Large S
Page 3 and 4: JUPITER JUPITER’S Four Largest Mo
Page 5 and 6: ZEUS and EUROPA Zeus was enamored o
Page 7 and 8: JUPITER and CALLISTO Callisto took
Page 9 and 10: The Large Moons Characteristics •
Page 11 and 12: Impacts and Cratering in the Outer
Page 13 and 14: Crater-Retention Ages on the Satell
Page 15 and 16: Crater-Retention Ages on the Satell
Page 17 and 18: Callisto: Basic Facts • Diameter
Page 19 and 20: First Look at Callisto Voyager
Page 21: Geology of Callisto • Very Little
Page 25 and 26: Ganymede 3rd Closest Moon to Jupite
Page 27 and 28: Ganymede: A Moon with a History •
Page 29 and 30: Ganymede • Old, Dark Terrains and
Page 31 and 32: Ganymede Indications of Internal Ac
Page 33 and 34: Anatomy of a Torn Comet Crater Chai
Page 35 and 36: • Smallest Galilean Satellite 3,1
Page 37 and 38: • Little Topographic Relief • S
Page 39 and 40: Europa • Scalloped Arc Shaped Pat
Page 41 and 42: Europa Close-Up of Chaotic Surface
Page 43 and 44: • Magnetic Field Indicates a Coup
Page 45 and 46: Io Density - 3.3 g/cm3 • Higher t
Page 47 and 48: 15.4 Io The Volcanic Moon • Surfa
Page 49 and 50: Io • About Same Distance as Moon
Page 51 and 52: Io • Water, Other Ices, Carbon, N
Page 53 and 54: Geology of Io High Resolution View
Page 55 and 56: Volcanic Eruption on JUPITERR’S M
Page 57 and 58: IO Plume Eruptions • 10 Tons/Sec
Page 59 and 60: Volcanic Eruption on JUPITERR’S M
Page 61 and 62: Io Infrared Emissions from Hot Spot
Page 63 and 64: Dione - Foreground, Tethys and Mima
Page 65 and 66: • Infrared Spectrum of Titan (top
Page 67 and 68: Titan Composition of the Atmosphere
Page 69 and 70: Photochemical Smog • Detached Lay
Page 71 and 72: Voyager Ultraviolet Spectrometer Re
Page 73 and 74:
Evolution of the Atmosphere • Met
Page 75 and 76:
SATURN Cassini Orbiter Remained in
Page 77 and 78:
TITAN Huygens Lander September 2004
Page 79 and 80:
NEPTUNE by Itself - Proved to Be
Page 81 and 82:
Triton (in Foreground) Large Moon
Page 83 and 84:
Triton (in Foreground) Retrograde O
Page 85 and 86:
Triton’s Surface Unique Surface A
Page 87 and 88:
Triton Nitrogen Atmosphere
Page 89 and 90:
• Calculations Based Upon the App
Page 91 and 92:
Evolution of the Atmosphere Geyser
Page 93 and 94:
Triton Moon of NEPTUNE Nitrogen Gey
Page 95 and 96:
15.7 Comparing the Large Satellites
Page 97 and 98:
Page 99 and 100:
Page 101 and 102:
Page 103 and 104:
Page 105 and 106:
Page 107 and 108:
Page 109 and 110:
Page 111 and 112:
1994 Galileo Spacecraft Launched To
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2500-15-large satellites

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