2500-15-large satellites

More documents

Recommendations

Info

<strong>15</strong>.7 Comparing the Large Satellites Ganymede and Callisto Why Did Ganymede Differentiate and Maintain a Substantial Level of Geological Activity for Millions of Years While Callisto Did Not ? Shown to Scale in this Composite Galileo Photograph
<strong>15</strong>.7 Comparing the Large Satellites Ganymede Is: • Closer to JUPITER – Subject to Larger Tidal Stress (Heating) • Subject to More Impacts Due to Attraction of JUPITER’S Gravity • Larger and Slightly Denser Than Callisto - Contains More Radioactive Materials (More Internal Heating) - Retains Heat Slightly Better Which Means Higher Internal Temperature and Slower Cooling 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
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 and 22:
Geology of Callisto • Very Little
Page 23 and 24:
• High-Resolution View of the Sur
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: 15.7 Comparing the Large Satellites
Page 99 and 100: 15.7 Comparing the Large Satellites
Page 111 and 112: 1994 Galileo Spacecraft Launched To
show all

2500-15-large satellites

Create successful ePaper yourself

Delete template?

Save as template?