Planetary Geology pdf - NASA

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c. The terms ÒsharpÓ and ÒsubduedÓ are descriptive terms, used to describe the morphologies of craters. Sharp-appearing craters are sometimes referred to as Òfresh,Ó while subdued-appearing craters are commonly referred to as Òdegraded.Ó What do the terms ÒfreshÓ and ÒdegradedÓ imply about how a craterÕs morphology changes with time on Rhea? 14. Notice that some of RheaÕs craters, including crater A, show central peaks. These form upon impact, due to rebound of the floor during the Òmodification stageÓ of the cratering process. a. On the acetate, outline as many central peak craters as you can confidently identify. Retain the scheme of outlining each sharp crater with a solid line, and each subdued crater with a dashed line. Put a dark dot in the middle of each central peak crater that you identify. b. Are central peaks more recognizable in sharp or subdued craters? c. Based on your answer to part b, what can you infer about how the topography of a central peak changes over time? d. Central peaks form only in craters above a certain diameter. This Òtransition diameterÓ from simple, bowl-shaped craters to more complex, central peak craters depends on surface gravity and material properties, so it is different for each planet and satellite. Estimate the transition diameter for craters on Rhea based on the smallest central peak craters that you are able to identify. 15. Consider the surface of Rhea (Figure 13.3) in comparison to the surfaces of Ganymede (Figure 13.1) and Enceladus (see Figure 13.3 and your sketch map). a. Compare and contrast the general appearance of the surface of Rhea to the surfaces of Ganymede and Enceladus. b. What do the differences in surface appearance suggest about the geological history of Rhea as compared to the histories of Ganymede and Enceladus? IV. Io 16. Io is a satellite of the planet __________. Its density of ______ g/cm3 means that it is composed of _____________________. This density is unusual in that it is ___________ than that of any other outer planet satellite. Io is _____________ km in radius. Examine Figure 13.4, which shows part of the surface of Io. The very high albedo material is considered to be sulfur dioxide frost. When the two Voyager spacecraft flew by Io in 1979, they photographed nine actively erupting volcanoes. 17. Examine the feature in the far northeast corner of the image, which shows a central depression with relatively low albedo (dark) material radiating from it. a. What process created this feature? Exercise Thirteen: The Geology of Outer Planet Satellites 159 EG-1998-03-109-HQ Activities in Planetary Geology for the Physical and Earth Sciences
. Describe in detail the shape of the central depression. Use a sketch if you like. (Use the sketch area below.) Sketch area c. What kind of volcanic ÒcraterÓ is this central depression? 18. Examine the other craters and surface features seen in Figure 13.4. What is the principal process shaping the surface of Io? List some observations that support your answer. 19. Contrast the characteristics of craters that you see on Io to those on Rhea. List at least four differences between IoÕs volcanic craters and RheaÕs impact craters. 20. On the chart below, rank the relative importance of impact cratering, volcanism, and tectonism on the four outer planet satellites that you have studied, based on the images you have seen. Use numbers from 1 (for the satellite most affected) to 4 (for the satellite least affected). Impact Cratering Volcanism Tectonism Ganymede Enceladus Rhea Io 160 Exercise Thirteen: The Geology of Outer Planet Satellites Activities in Planetary Geology for the Physical and Earth Sciences EG-1998-03-109-HQ
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National Aeronautics and Space Admi
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A ctivities in Planetary Geology fo
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Preface Introduction Special Note t
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We are living in a time of revoluti
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Exercise One Suggested Correlation
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Part One 1. (Answers will vary.) Vo
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5. Based on the number of pictures
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_____ 08/19/92 earthquake, central
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165° W 75°W 0° 75°E180°E 75°N
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1. a. The volcano has a circular ba
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Exercise Two Volcanism Purpose By s
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7. List some factors that might aff
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. How is it similar? Examine the vi
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N 200 m Figure 2.1. Mount Capulin,
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N Figure 2.3. Oblique aerial view o
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Figures 2.7.a., 2.7.b. Meteor Crate
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N Figure 2.9. Mosaic of Landsat fra
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1. a. Sketch should show steep side
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Exercise Three Purpose By using ste
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Gradation 2. Figure 3.4 shows a por
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. Examine the broad, steep face tha
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e. Determine the sequence of events
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Exercise Three: Geologic Landforms
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Exercise Three: Geologic Landforms
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N Figure 3.8. Sierra Caballos Mount
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Exercise Four Impact Cratering Inst
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Objective To determine the initial
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Name Exercise Four Impact Cratering
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Sketch area In the fourth section o
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Part C Shot 1 (smallest) Shot 2 (ne
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10 km Exercise Four: Impact Crateri
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Science Standards ■ Earth and Spa
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Figure 5.1. Comparison of the forma
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Exercise Five Purpose To illustrate
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Part B: Volcanic Explosive Craterin
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N 100 km Figure 5.5. Olympus Mons,
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Exercise Six Suggested Correlation
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Figure 6.1. Different sand surfaces
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Exercise Six Purpose To learn how p
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*c. What geologic process(es) forme
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Figure 6.4. Photograph of lunar mar
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Exercise Seven Coriolis Effect Inst
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Purpose By tracing an object as it
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N 100 km Figure 7.1. Centered at 20
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elow this is the solid core of the
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for turbulent, inclement weather on
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7. Examine the atmosphere of Venus
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Figure 8.5. Viking Orbiter image 78
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N 102 Figure 8.7. Jupiter as seen b
Page 99 and 100: emove the flaps). Three windows are
Page 101 and 102: Purpose In this experiment you will
Page 103 and 104: 10. Based on your three sketches of
Page 105 and 106: The wind is at work on other planet
Page 107 and 108: Unit Four The three decades from th
Page 109 and 110: 1. The highlands are bright, rugged
Page 111 and 112: 6. Based on the number of craters,
Page 113 and 114: Mercury Venus Earth Moon Mars Mean
Page 115 and 116: Figure 10.2. Mariner 10 mosaic of M
Page 117 and 118: C Figure 10.4. Magellan radar mosai
Page 119 and 120: Exercise Eleven Suggested Correlati
Page 121 and 122: Exercise Eleven Purpose To learn to
Page 123 and 124: . If windstreaks are dust deposits
Page 125 and 126: Figure 11.2. Ius Chasma, part of th
Page 127 and 128: Exercise Eleven: Geologic Features
Page 129 and 130: Exercise Twelve Suggested Correlati
Page 131 and 132: Exercise Twelve Purpose To learn ab
Page 133 and 134: So far all the figures have shown f
Page 135 and 136: Figure 12.3. The prominent circular
Page 137 and 138: N 100 km Figure 12.6. Volcanoes com
Page 139 and 140: Exercise Twelve: Geologic Features
Page 141 and 142: Exercise Thirteen Suggested Correla
Page 143 and 144: I. Ganymede 1. Ganymede orbits the
Page 145 and 146: 17. a. Volcanism. b. It shows a som
Page 147 and 148: Properties of the Major Satellites*
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Page 155 and 156: A Figure 13.3. The surface of Rhea,
Page 157 and 158: Exercise Fourteen Planets in Stereo
Page 159 and 160: Exercise Fourteen: Planets in Stere
Page 161 and 162: 9. Examine the stereo images of Fig
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Page 167 and 168: Exercise Fourteen: Planets in Stere
Page 169 and 170: 25 km Figure 14.10. The icy uranian
Page 171 and 172: Exercise Fifteen Suggested Correlat
Page 173 and 174: Exercise Fifteen Purpose The object
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Page 177 and 178: Figure 15.1. Sample geologic map an
Page 179 and 180: Figure 15.3. Apollo 15 photograph o
Page 181 and 182: Part A 1. Contacts are sharp; trans
Page 183 and 184: Geologic History Youngest Youngest
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Page 187 and 188: To establish age relations and inte
Page 189 and 190: Figure 16.1. Sample geologic map an
Page 191 and 192: Figure 16.3. Diagram of typical imp
Page 193 and 194: Exercise Sixteen: Photogeologic Map
Page 195 and 196: Figure 16.8. Northwest quadrant of
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Answer Key Map after 1) Scott et al
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Exercise Seventeen Purpose Through
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Figure 17.2. Sample geologic map an
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Geologic History: Youngest Oldest E
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Erosion: Process whereby materials
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Terrain: A region of a surface shar
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Cattermole, P. (1994). Venus: The G
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Object Moon Moon Moon Moon Moon Moo
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Object Jupiter Jupiter Jupiter Jupi
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1.6 Regional Planetary Image Facili
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2. Map Link 25 Eat Mason Santa Barb
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NATIONAL AERONAUTICS AND SPACE ADMI
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