2500-15-large satellites

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<strong>15</strong>.7 Comparing the Large Satellites Titan Point #4 The Ability of Water Ice to Trap Gases Depends Upon the Temperature of the Ice (and Therefore the Structure), Along With the Size and Electrical Properties of the Gas Molecules • Hydrogen (H), Helium (He) and Neon (Ne) Are Only Trapped at Temperatures Below 25 o K • Argon (Ar), Methane (CH 4 ), Nitrogen (N 2 ), and Carbon Monoxide (CO) Are Trapped in Varying Amounts Depending on the Ice Temperature
<strong>15</strong>.7 Comparing the Large Satellites Titan Point #4 The Jovian Satellites Were Simply Too Warm for Ice to Trap Any of These Gases (Closer to the Sun and Tidal Heating by JUPITER) • Titan, SATURN’S Largest Satellite, Is Farther Away from the SUN, and Does Not Experience Tidal Heating to the Degree of the Jovian Satellites • Titan’s Gas-Rich Ice Was Able to Condense and Serve as the Carrier of Nitrogen and Other Volatiles Found on the Satellite
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Worlds of Fire and Ice: The Large S
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JUPITER JUPITER’S Four Largest Mo
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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
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Crater-Retention Ages on the Satell
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Callisto: Basic Facts • Diameter
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First Look at Callisto Voyager
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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
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Europa • Scalloped Arc Shaped Pat
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Europa Close-Up of Chaotic Surface
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• Magnetic Field Indicates a Coup
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Io Density - 3.3 g/cm3 • Higher t
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15.4 Io The Volcanic Moon • Surfa
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Io • About Same Distance as Moon
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Io • Water, Other Ices, Carbon, N
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Geology of Io High Resolution View
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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 107: 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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