2500-15-large satellites

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<strong>15</strong>.7 Comparing the Large Satellites Ganymede • These Factors Are Small – But Even When Taken Together - They Would Not Produce Differentiation on Their Own • Rather - They Triggered a Major Change in Another Internal Process – Possibly Upper Mantle Convection • Sufficient to Drive Early Plate Tectonics for 1 Billion Years • Finally - Cooling Produced a Phase Change of Interior Liquid Water to Solid Ice - Crust Cracked with Minor Mountain Building Shown to Scale in this Composite Galileo Photograph
<strong>15</strong>.7 Comparing the Large Satellites Europa and Io Why Are Europa and Io So Depleted in Water and Other Volatiles Relative to Callisto and Ganymede ? Shown to Scale in this Composite Galileo Photograph
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
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JUPITER and CALLISTO Callisto took
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The Large Moons Characteristics •
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Impacts and Cratering in the Outer
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Crater-Retention Ages on the Satell
Page 15 and 16:
Crater-Retention Ages on the Satell
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Callisto: Basic Facts • Diameter
Page 19 and 20:
First Look at Callisto Voyager
Page 21 and 22:
Geology of Callisto • Very Little
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• High-Resolution View of the Sur
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Ganymede 3rd Closest Moon to Jupite
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Ganymede: A Moon with a History •
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Ganymede • Old, Dark Terrains and
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Ganymede Indications of Internal Ac
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Anatomy of a Torn Comet Crater Chai
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• Smallest Galilean Satellite 3,1
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• Little Topographic Relief • S
Page 39 and 40:
Europa • Scalloped Arc Shaped Pat
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Europa Close-Up of Chaotic Surface
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• 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: 15.7 Comparing the Large Satellites
Page 111 and 112: 1994 Galileo Spacecraft Launched To
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2500-15-large satellites

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