Planetary Geology pdf - NASA

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Exercise Ten Suggested Correlation of Topics Purpose The objective of this exercise is to recognize and compare the similarities and differences among the surfaces of the terrestrial planets at a global scale. Materials Suggested: clear acetate or overhead transparency film, overhead projector markers, metric ruler, drawing compass (a single compass can be used by a group of students). Substitutions: tracing paper, colored pens or pencils, pen and string (as a compass). Background This exercise views Mercury, Venus, Earth, Moon, and Mars at the global scale. At this scale only the largest and most prominent landforms and terrains Exercise Ten: Landform Mapping: The Terrestrial Planets Exercise Two is suggested as an introductory exercise. Planetary comparisons, geomorphology Landform Mapping: The Terrestrial Planets Instructor Notes 115 are visible. This provides a starting point for more detailed study of planetary surfaces in later exercises or as provided by the instructor. Note that the Moon, although not actually a planet, is typically grouped with the terrestrial planets when considering its geology. This exercise is best worked in pairs or small groups of students. When the students are working on question 16, encourage them to compare the images side by side in ordering the surfaces from least to most complex. The starred question can be used for more advanced students or for class discussion. Science Standards ■ Earth and Space Science ¥ Origin and evolution of the Earth system Mathematics Standards ■ Connections ■ Number and number relationships EG-1998-03-109-HQ Activities in Planetary Geology for the Physical and Earth Sciences 1.5 hours
1. The highlands are bright, rugged and heavily cratered. The plains are dark, flat, smooth and less cratered. 2. The highlands. 3. The highlands. 4. Younger. 5. Cratered plains and rayed craters. 6. Older than the lunar plains. (Lunar plains are often called maria.) 7. All three surfaces have craters, although Mars has the least. Mars has more extensive smooth plains than the Moon or Mercury; no obvious volcanoes or canyons are visible on either Mercury or the Moon. Only Mars shows polar ice caps. 8. Mars has a dynamic atmosphere (including dust storms). Gradation by running water occurred on Mars, but water never flowed on the Moon. Volcanic activity has been more extensive on Mars. Tectonism has occurred on Mars. On the Moon, impact cratering and plains volcanism have been the major geologic processes; on Mars, all four major geologic processes have worked to shape the surface. 9. Younger. 10. The southern region is older. 11. Mars. 12. a. Both are long and relatively narrow. The canyon on Mars is straight, the one on Venus is arcuate. [If the student says the Venus canyon is bright and the Mars canyon is dark, remind them of the differences in imaging systems: radar vs. optical camera.] 13. Younger. 14. a. Smooth plains, canyons (deep ocean trenches and rifts in Africa), volcanoes (represented by islands) and rough ÒhighlandsÓ (mountain ranges). b. Continents, mid-ocean rift/ridge zones. 15. a. Similarities: if EarthÕs continents are thought of as Òhighlands,Ó both can be divided into highÐ and low-standing regions; low-lying regions are relatively smooth. Differences: the Moon is dominated by craters; lowlands on the Moon are formed by large impacts flooded Answer Key 116 by volcanic material; no linear mountain chains on the Moon; no prominent arcuate ridges or trenches on the Moon. b. Students will have difficulty finding any similarities between Earth and Mercury. Differences: Mercury is dominated by craters (impact cratering is the prominent geologic process); on this image of the Earth, impact cratering is the only geologic process that is not apparent. c. Similarities: both have volcanic and tectonic landforms. Differences: no continents or midocean ridge system on Mars, no craters seen on this global view of Earth. d. Similarities: both show arcuate mountain ranges; both show expansive smooth regions; neither shows very large craters. Differences: more extreme topography on Earth, continents and deep ocean basins, compared to more uniform topographic level on Venus; no midocean ridge systems on Venus. 16. a. Oldest to youngest: Mercury, Moon, Mars, Venus, Earth. b. Answers will vary based on students perception of Òmost complex.Ó Earth has the most active geologic history reflected on its surface, however, some students may argue that Venus is more complex. Least to most complex: Mercury, the Moon, Mars, Venus, Earth. 17. (This representation is ~1/3 the size of what student answer should be.) Moon Mercury Mars Venus Earth *18. Answers may vary. In general it is true that the larger the terrestrial planet, the more complex its surface. This is not strictly true, however: the Moon, despite its smaller size, is arguably more complex than Mercury. Students might wish to debate the relative complexity of Earth and Venus, or Venus and Mars, as seen at the global scale. Exercise Ten: Landform Mapping: The Terrestrial Planets 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
Page 57 and 58: Sketch area In the fourth section o
Page 59 and 60: Part C Shot 1 (smallest) Shot 2 (ne
Page 61 and 62: 10 km Exercise Four: Impact Crateri
Page 63 and 64: Science Standards ■ Earth and Spa
Page 65 and 66: Figure 5.1. Comparison of the forma
Page 67 and 68: Exercise Five Purpose To illustrate
Page 69 and 70: Part B: Volcanic Explosive Craterin
Page 71 and 72: N 100 km Figure 5.5. Olympus Mons,
Page 73 and 74: Exercise Six Suggested Correlation
Page 75 and 76: Figure 6.1. Different sand surfaces
Page 77 and 78: Exercise Six Purpose To learn how p
Page 79 and 80: *c. What geologic process(es) forme
Page 81 and 82: Figure 6.4. Photograph of lunar mar
Page 83 and 84: Exercise Seven Coriolis Effect Inst
Page 85 and 86: Purpose By tracing an object as it
Page 87 and 88: N 100 km Figure 7.1. Centered at 20
Page 89 and 90: elow this is the solid core of the
Page 91 and 92: for turbulent, inclement weather on
Page 93 and 94: 7. Examine the atmosphere of Venus
Page 95 and 96: Figure 8.5. Viking Orbiter image 78
Page 97 and 98: 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: Unit Four The three decades from th
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*
Page 149 and 150: The surface of Enceladus can be div
Page 151 and 152: . Describe in detail the shape of t
Page 153 and 154: Figure 13.1.b. Geological sketch ma
Page 155 and 156: A Figure 13.3. The surface of Rhea,
Page 157 and 158: Exercise Fourteen Planets in Stereo
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Exercise Fourteen: Planets in Stere
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9. Examine the stereo images of Fig
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. Sketch what a profile across a ty
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5 km Figure 14.3. Crater Geopert-Me
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Exercise Fourteen: Planets in Stere
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25 km Figure 14.10. The icy uranian
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Exercise Fifteen Suggested Correlat
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Exercise Fifteen Purpose The object
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3. What is the age relation between
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Figure 15.1. Sample geologic map an
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Figure 15.3. Apollo 15 photograph o
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Part A 1. Contacts are sharp; trans
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Geologic History Youngest Youngest
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Exercise Sixteen Purpose Through ob
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To establish age relations and inte
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Figure 16.3. Diagram of typical imp
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Exercise Sixteen: Photogeologic Map
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Figure 16.8. Northwest quadrant of
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Figure 16.10. Southeast quadrant of
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Youngest Youngest Oldest Oldest Fig
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Answer Key Map after 1) Scott et al
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Exercise Seventeen Purpose Through
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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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