Planetary Geology pdf - NASA

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1. It is approximately circular, but has numerous over-lapping craters within it and at the margins. 2. Answers will vary, but should include: a) erosion, b) tectonism (faulting). 3. Geologically young because there are few impact craters. Younger than the surface of the moon. 4. Answers will vary. The sharp, straight cliffs and the large dimensions suggest tectonic processes; the stream patterns on the south side are indicative of modification by running water. 5. Ius Chasma is larger by several times. 6. a. Northeast (to the top of the photo). b. Craters are numerous and degraded, indicating this is a relatively ancient region. c. The craters are older than the valleys which cut across the center rims. However, there are also a few fresh, young craters superposed on the channels, indicating that these impacts occurred after channel formation. 7. a. The diffuse streaks of bright material are found on the southeast side of craters. b. The wind blew from the northwest. Answer Key 128 8. a. Like Olympus Mons, Apollinaris Patera has radial flow patterns and a basal scarp (cliff). Apollinaris Patera has more craters, a large flow trending to the south, and a less complex caldera than that of Olympus Mons. Olympus Mons is a much larger edifice. b. Volcanism, considering its characteristics described above. c. Impact formed Reuyl crater, indicated by the ejecta pattern and central peak. d. Gradation by running water, indicated by the meandering pattern and tributary channels. e. Water that once flowed through MaÕadim Vallis may have deposited sedimentary material onto the floor of Gusev crater. 9. Answers will vary. D, A (C), C (A), B. D is a very old degraded crater. The flows from A are modified at their southern part by sediments from crater D due to flow of water in channel C. So A preceded C. (This is very difficult to see and students may reverse the order of these two events.) Crater B is fresh in appearanceÑrim is not erodedÑand thus is probably very young. Exercise Eleven: Geologic Features of Mars Activities in Planetary Geology for the Physical and Earth Sciences EG-1998-03-109-HQ
Exercise Eleven Purpose To learn to identify landforms on the surface of Mars and the geological processes that produced them. Introduction In many ways Mars is similar to Earth. The same four geologic processes that shape EarthÑgradation, impact cratering, tectonism, and volcanismÑ have left their mark on Mars. Volcanism has produced vast lava flows, broad shield volcanoes, and plains of volcanic material. Mars has some of the largest volcanoes in the solar system, including Olympus Mons, a massive volcano many times larger than the Island of Hawaii. Olympus Mons is only one of four huge volcanoes in a 3000 km-wide region called Tharsis. These volcanoes erupted repeatedly over many millions of years, growing higher with each lava flow. Enormous collapse calderas are found on the summits of each of the volcanoes. Gradation is the dominant geologic process acting on Mars today. Mass movement is the displacement of material by landslides or slumping through the action of gravity. Aeolian (wind) activity is also a continuing process of gradation. Sand and dust particles carried by the wind form dunes and windstreaks. Although temperatures below freezing and low atmospheric pressures do not allow liquid water on the surface of Mars today, gradation processes involving running water were important on Mars in the past. Valley systems cut through many of the cratered terrains of Mars and have characteristics analogous to water-cut valleys on Earth. Exercise Eleven: Geologic Features of Mars Name Geologic Features of Mars 129 A mystery concerning water on Mars is ÒWhere did it go?Ó Some water probably seeped into the ground and is frozen there today as ice, and some likely escaped into space over time. Moreover, the polar caps contain some water ice. Mars, like the Earth, has seasons. The polar caps shrink during local summer and grow during local winter. Although Mars does not have plate tectonics like the Earth, there are many tectonic features that show its surface has been deformed. Stresses can be caused by subsurface uplift or by the addition of mass (such as lava flows) that weigh down an area. Extensional stresses have led to the formation of great valleys such as Valles Marineris, the longest canyon system in the solar system. As on the Moon, Mercury, Venus, and most of the outer planet satellites, impact craters are found on the surface of Mars. Craters can be used to determine the relative ages of martian surface materials; in general, older surfaces have craters which are more numerous, larger, and more degraded than those on young surfaces. Moreover, the principles of superposition and cross-cutting relations indicate that a feature which at least partly covers another feature is the younger. Thus, if a valley cuts through a crater, the crater must be older. Individual craters are degraded or destroyed over time by gradational processes and further cratering. Therefore, crisp craters with upraised rims and steep sides are young, while less distinct and eroded craters with partial rims are probably older. Through a combination of these principles, the relative ages of geologic features can be determined, and a sequence of geologic events developed. EG-1998-03-109-HQ Activities in Planetary Geology for the Physical and Earth Sciences
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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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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
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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
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: Exercise Eleven Suggested Correlati
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
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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
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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
Page 159 and 160: Exercise Fourteen: Planets in Stere
Page 161 and 162: 9. Examine the stereo images of Fig
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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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