Planetary Geology pdf - NASA

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1. a. Answers will vary, student may say in straight lines or arcs. b. (See Figure 5.1) The formation of an impact crater is a relatively well ordered event in which the ejecta leaves the surface at approximately a 45¡ angle from the horizontal (upper left picture Figure 5.1). As the crater enlarges (middle left), the inverted cone sheet of ejecta, called the ejecta plume, enlarges. Ejecta falls first close to the crater, and as crater formation continues (bottom left), the ejecta strike the surface at increasing distances. Note how the base of the ejecta plume has enlarged with time. 2. a. Ejecta from the vertical impact are thrown out at about a 45¡ angle. The sheet of ejecta moves outward in a symmetrical pattern, producing the appearance of an enlarging, inverted cone. For the 45¡ impact, the ejecta cone becomes asymmetrical and distorted in the down-range direction. b. (See Figure 5.2) As the angle of impact departs from the vertical, the ejecta cone or plume becomes asymmetric. For the relatively low velocities represented in the figure (20 m/s), asymmetry is not apparent until the impact angle is greater than 20¡. At 20¡ (upper right), the sequence of ejecta remains relatively symmetric. At 60¡ (lower left) and 75¡ (lower right) from the vertical, the ejecta cone is distorted in the downrange direction. For impacts of much greater velocities (2 km/s), the asymmetry does not occur until much larger departures (80¡) from the vertical. 3. a. (See Figure 5.1.) The upper and middle right pictures in the figure show the relatively chaotic and dispersed nature of the ejecta caused by this type of cratering process. Exercise Five: Comparative Cratering Processes Answer Key EG-1998-03-109-HQ Activities in Planetary Geology for the Physical and Earth Sciences 65 b. In appearance, the crater shape is similar. However, the ejecta pattern is chaotic and dispersed with ejecta thrown at all angles. Note that the ejecta pattern and crater appearance will vary with different depths of burial of the balloon. 4. (See Figure 5.1) The bottom right picture shows the formation of the eruptive crater. Ejecta is blown straight up and lands right around the crater. 5. a. All three craters contain similar parts: crater, rim, ejecta. b. Answers will vary, but many students will note that the explosive and volcanic craters are not as symmetrical as the impact craters. The volcanic eruption crater will be the most irregular. c. All craters formed have raised rims. d. Answers may vary. The crater ejecta patterns will probably be widest. e. Impact has the greatest effect. 6. a. Olympus Mons (Figure 5.5) is volcanic; Timocharis crater (Figure 5.6) is of impact origin. b. Timocharis has well developed ejecta patterns; the crater on Olympus Mons is irregular in outline and shows no ejecta patterns. c. Impact craters have large, well-defined ejecta patterns; the ejecta patterns of volcanic explosion craters may not be as well-organized; volcanic eruption craters have little ejecta or poorly organized ejecta patterns.
Figure 5.1. Comparison of the formation of an impact crater (left side), a low-energy explosion crater (top two photos on the right side), and simulated volcanic eruptive crater (bottom right). All craters were formed in a sand box and recorded using a strobe light. 66 Exercise Five: Comparative Cratering Processes 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
Page 13 and 14: 5. Based on the number of pictures
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Page 19 and 20: 1. a. The volcano has a circular ba
Page 21 and 22: Exercise Two Volcanism Purpose By s
Page 23 and 24: 7. List some factors that might aff
Page 25 and 26: . How is it similar? Examine the vi
Page 27 and 28: N 200 m Figure 2.1. Mount Capulin,
Page 29 and 30: N Figure 2.3. Oblique aerial view o
Page 31 and 32: Figures 2.7.a., 2.7.b. Meteor Crate
Page 33 and 34: N Figure 2.9. Mosaic of Landsat fra
Page 35 and 36: 1. a. Sketch should show steep side
Page 37 and 38: Exercise Three Purpose By using ste
Page 39 and 40: Gradation 2. Figure 3.4 shows a por
Page 41 and 42: . Examine the broad, steep face tha
Page 43 and 44: e. Determine the sequence of events
Page 45 and 46: Exercise Three: Geologic Landforms
Page 47 and 48: Exercise Three: Geologic Landforms
Page 49 and 50: N Figure 3.8. Sierra Caballos Mount
Page 51 and 52: Exercise Four Impact Cratering Inst
Page 53 and 54: Objective To determine the initial
Page 55 and 56: 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: Science Standards ■ Earth and Spa
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 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
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Figure 10.2. Mariner 10 mosaic of M
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C Figure 10.4. Magellan radar mosai
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Exercise Eleven Suggested Correlati
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Exercise Eleven Purpose To learn to
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. If windstreaks are dust deposits
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Figure 11.2. Ius Chasma, part of th
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Exercise Eleven: Geologic Features
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Exercise Twelve Suggested Correlati
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Exercise Twelve Purpose To learn ab
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So far all the figures have shown f
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Figure 12.3. The prominent circular
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N 100 km Figure 12.6. Volcanoes com
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Exercise Twelve: Geologic Features
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Exercise Thirteen Suggested Correla
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I. Ganymede 1. Ganymede orbits the
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17. a. Volcanism. b. It shows a som
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Properties of the Major Satellites*
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The surface of Enceladus can be div
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. Describe in detail the shape of t
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Figure 13.1.b. Geological sketch ma
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A Figure 13.3. The surface of Rhea,
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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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