Botkin Environmental Science Earth as Living Planet 8th txtbk

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436 CHAPTER 20 The Atmosphere, Climate, and Global Warming each hemisphere (see Figure 20.7 for more details). In general belts of low air pressure develop at the equator where the air is warmed most of the time during the day by the sun. The heated air rises, creating an area of low pressure and a cloudy and rainy climate (cell 1 Figure 20.7). This air then moves to higher latitudes (toward the poles), and because it is cooler at higher elevations and because sunlight is less intense at the higher latitudes. By the time the air that was heated at the equator reaches about 30 latitude, it has cooled enough to become heavier, and it descends, creating a region of high pressure, with its characteristic sunny skies and low rainfall, forming a latitude belt where many of the world’s deserts are found. Then the air that descended at 30 latitude moves poleward along the surface warms and rises again, creating another region of generally low pressure around 50 to 60 (cell 2, Figure 20.7) latitude and once again becoming a region of clouds and precipitation. Atmospheric orientation in cell 3 (Figure 20.7) moves air toward the poles at higher elevation and toward the equator along the surface. Sinking cool air at the poles produces the polar high-pressure zones at both poles. At the most basis level warm air rises at the equator moves toward the poles where it sinks after going through (cell 2) and return flow is along the surface of Earth toward the equator. Of course, the exact locations of the areas of rising (low-pressure) and falling (high-pressure) air vary with the season, as the sun’s position moves north and south relative to the Earth’s surface. You can begin to understand that what would seem at first glance to be just a simple container of gases has complicated patterns of movement and that these change all the time for a variety of reasons. The latitudinal belts (cells) just described have names, most of which came about during the days of sailing ships. Such names include the “doldrums,” regions at the equator with little air movement; “trade winds,” northeast and southeast winds important when clipper ships moved the world’s goods; and “horse latitudes,” two belts centered about 30° north and south of the equator with descending air and high pressure. Energy and the Atmosphere: What Makes the Earth Warm Almost all the energy the Earth receives is from the sun (a small amount comes from the interior of the Earth and an even smaller amount from frictional forces due to the moon revolving around the Earth). Sunlight comes in a wide range of electromagnetic radiation, from very long radio waves to much shorter infrared waves, then shorter wavelengths of visible light, even shorter wavelengths Wavelength 10 5 m 10 4 m 10 3 m 10 2 m 10 m 1 m 10 cm 1 cm 10 – 1 cm 100 m 10 m 1 m 10 – 1 m 10 – 2 m 10 – 3 m 10 – 4 m Long radio waves AM radio Shortwave radio Infrared Ultraviolet 1 μm = 10 – 6 m = 1 micron Microwaves Visible X rays Gamma rays 0.7 μm Red 0.6 μm Orange Yellow 0.5 μm Green Blue 0.4 μm Violet FIGURE 20.8 Kinds of electromagnetic radiation the Earth receives. of ultraviolet, and then on to shorter and shorter wavelengths (Figure 20.8). Most of the sun’s radiation that reaches the Earth is in the visible and near infrared wavelengths (Figure 20.9), while the Earth, much cooler, radiates energy mostly in the far infrared, which has longer wavelengths. (The hotter the surface of any object, the shorter the dominant wavelengths. That’s why a hot flame is blue and a cooler flame red.) Under typical conditions, the Earth’s atmosphere reflects about 30% of the electromagnetic (radiant) energy that comes in from the sun and absorbs about 25%. The remaining 45% gets to the surface (Figure 20.10). As the surface warms up, it radiates more energy back to the atmosphere, which absorbs some of it. The warmed atmosphere radiates some of its energy upward into outer space and some downward to the Earth’s surface.
20.4 The Atmosphere 437 Sun (5800°C) Relatively short-wave radiation from sun (mostly visible) Earth (15°C) Relatively long-wave radiation from Earth (mostly infrared) Sun Peaks in the visible light spectra Radiation flux (W/m 2 /μm) 10 5 10 3 10 1 Earth 10 7 0.01 0.1 1 10 100 1000 Radiation flux is a million (10 6 ) times greater for the sun than the Earth All in infrared part of spectrum 10 –1 Wavelength (μm) FIGURE 20.9 The sun, much hotter than the Earth, mostly emits energy in the visible and near infrared. The cooler Earth emits energy mostly in the far (longer-wavelength) infrared. 100% Incoming solar radiation 30% Reflected to space (25% from atmosphere, 5% from surface of Earth) 100% Total outgoing infrared radiation (earthshine) 70% Heat lost to space (from atmosphere and surface of Earth) 25% Absorbed in atmosphere 45% Absorbed by Earth at surface Heat reabsorbed by Earth (CO 2 ,CH 4 , etc.) FIGURE 20.10 Earth’s energy budget.
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ENVIRONMENTAL SCIENCE Earth as a Li
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VICE PRESIDENT AND EXECUTIVE PUBLIS
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About the Authors Daniel B. Botkin
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Preface vii Themes Our book is base
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Preface ix Updated Critical Thinkin
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Acknowledgments Reviewers of This E
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Acknowledgments xiii Karen Swanson,
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Contents Chapter 1 Key Themes in En
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xviii Contents Summary 125 Reexamin
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xx Contents Chapter 13 Wildlife, Fi
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xxii Contents CRITICAL THINKING ISS
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xxiv Contents Availability and Use
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2 CHAPTER 1 Key Themes in Environme
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10 CHAPTER 1 Key Themes in Environm
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over 4 million in 1950. In 1999 Tok
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CHAPTER 2 Science as a Way of Knowi
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24 CHAPTER 2 Science as a Way of Kn
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42 CHAPTER 3 The Big Picture: Syste
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60 CHAPTER 4 The Human Population a
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CHAPTER 5 Ecosystems: Concepts and
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82 CHAPTER 5 Ecosystems: Concepts a
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100 CHAPTER 5 Ecosystems: Concepts
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102 CHAPTER 5 Ecosystems: Concepts
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CHAPTER 6 The Biogeochemical Cycles
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106 CHAPTER 6 The Biogeochemical Cy
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128 CHAPTER 7 Dollars and Environme
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144 CHAPTER 8 Biological Diversity
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170 CHAPTER 9 Ecological Restoratio
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186 CHAPTER 10 Environmental Health
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212 CHAPTER 11 Agriculture, Aquacul
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236 CHAPTER 12 Landscapes: Forests,
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258 CHAPTER 13 Wildlife, Fisheries,
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CHAPTER 14 Energy: Some Basics LEAR
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288 CHAPTER 14 Energy: Some Basics
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304 CHAPTER 15 Fossil Fuels and the
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CHAPTER 16 Alternative Energy and t
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328 CHAPTER 16 Alternative Energy a
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346 CHAPTER 17 Nuclear Energy and t
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CHAPTER 18 Water Supply, Use, and M
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370 CHAPTER 18 Water Supply, Use, a
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486 CHAPTER 21 Air Pollution Table
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490 CHAPTER 21 Air Pollution chimn
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494 CHAPTER 21 Air Pollution SUMMAR
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496 CHAPTER 21 Air Pollution STUDY
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498 CHAPTER 22 Urban Environments C
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500 CHAPTER 22 Urban Environments I
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502 CHAPTER 22 Urban Environments o
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504 CHAPTER 22 Urban Environments K
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506 CHAPTER 22 Urban Environments 2
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508 CHAPTER 22 Urban Environments A
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510 CHAPTER 22 Urban Environments F
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512 CHAPTER 22 Urban Environments F
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518 CHAPTER 22 Urban Environments S
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520 CHAPTER 23 Materials Management
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552 CHAPTER 24 Our Environmental Fu
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Appendix A Special Feature: Electro
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Appendix A-3 VOLUME in 3 ft 3 yd 3
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Appendix A-5 Basic Chemistry
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Photo Credits CHAPTER 1 Ch Op 1: Im
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Glossary Abortion rate The estimate
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Glossary G-3 deposition of crustal
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Glossary G-5 high and the growth ra
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Glossary G-7 environmental impacts
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Glossary G-9 per unit time and some
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Glossary G-11 cooler than it is tod
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Glossary G-13 Nonpoint sources Poll
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Glossary G-15 Positive feedback A t
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Glossary G-17 Shelterwood cutting A
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Glossary G-19 Time series The set o
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Index Entries followed by an f may
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INDEX I-3 Sweetwater Marsh National
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INDEX I-5 dune succession, 96, 96f
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INDEX I-7 Colorado River, 114, 115f
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INDEX I-9 Lovelock, James, 10, 108
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INDEX I-11 Pelagic ecosystem, 85, 8
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INDEX I-13 Static systems, 44, 44f
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INDEX I-15 Watts, 291, 292t Weather
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N-2 NOTES 7. Schmidt, W.E. 1991 (Se
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N-4 NOTES 4. Christian, D. 2004. Ma
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N-6 NOTES 9. Collins, S.L., A.K. Kn
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N-8 NOTES 8. U.S. Department of Agr
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N-10 NOTES 19. O’Donnell, James J
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N-12 NOTES 19. Piore, 2002 (April 1
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N-14 NOTES application of secondary
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N-16 NOTES 22. Foukal, P., C. Frohl
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N-18 NOTES 54. Zummo, S.M., and M.H
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N-20 NOTES 38. Bullard, R.D. 1990.
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