Preface |
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xi | |
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1 | (14) |
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Past Thinking about Earth-Like Planets and Life |
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3 | (12) |
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The Habitable Zone and the Importance of Liquid Water |
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5 | (4) |
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Carl Sagan and the Drake Equation |
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9 | (2) |
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Other Perspectives on Planetary Habitability: Rare Earth and Gaia |
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11 | (4) |
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Part II: Our Habitable Planet Earth |
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15 | (82) |
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Critical Updates on How Planets Are Built |
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17 | (15) |
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The Conventional Wisdom regarding Planet Formation |
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18 | (3) |
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Where Did Earth's Water Come From? |
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21 | (2) |
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New Models for Planetary Accretion and Delivery of Water |
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23 | (2) |
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Could Earth's Water Have Come from Comets? |
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25 | (3) |
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An Up-to-Date Simulation of Planetary Accretion |
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28 | (4) |
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Long-Term Climate Stability |
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32 | (25) |
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32 | (4) |
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36 | (1) |
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Electromagnetic Radiation and the Greenhouse Effect |
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37 | (4) |
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41 | (1) |
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The Faint Young Sun Problem |
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42 | (3) |
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Possible Solutions to the Problem |
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45 | (4) |
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The Carbonate-Silicate Cycle and Controls on Atmospheric CO2 |
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49 | (4) |
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The CO2-Climate Feedback Loop |
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53 | (4) |
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More Wrinkles in Earth's Climate History |
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57 | (23) |
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The Phanerozoic Climate Record |
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58 | (5) |
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63 | (2) |
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Geologic Evidence for the Rise of Atmospheric O2 |
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65 | (3) |
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Cause of the O2 Rise: Cyanobacteria |
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68 | (3) |
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Methane, Methanogens, and the Universal Tree of Life |
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71 | (4) |
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The Archean Methane Greenhouse |
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75 | (2) |
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The Paleoproterozoic Glaciation |
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77 | (3) |
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Runaway Glaciation and ``Snowball Earth'' |
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80 | (17) |
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Milankovitch Cycles and the Recent Ice Ages |
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81 | (5) |
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Ice Albedo Feedback and Climatic Instability |
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86 | (2) |
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Evidence for Low-Latitude Glaciation |
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88 | (2) |
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Mechanisms for Explaining Low-Latitude Glaciation |
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90 | (2) |
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92 | (5) |
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Part III: Limits to Planetary Habitability |
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97 | (98) |
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Runaway Greenhouses and the Evolution of Venus' Atmosphere |
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99 | (17) |
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The History of Water on Venus |
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100 | (3) |
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The Classical Runaway Greenhouse Effect |
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103 | (3) |
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An Alternative Runaway Greenhouse Model |
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106 | (5) |
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Evolution of Venus' Atmosphere |
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111 | (5) |
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The Future Evolution of Earth |
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116 | (9) |
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High-CO2 Atmospheres and Temperature Limits for Life |
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116 | (2) |
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Future Solar Evolution and Lifetime of the Biosphere |
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118 | (3) |
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A Geoengineering Solution to Solar Luminosity Increases |
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121 | (4) |
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The Martian Climate Puzzle |
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125 | (22) |
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Evidence for Liquid Water near Mars' Surface |
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126 | (4) |
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130 | (1) |
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Evidence That Water Flowed in Mars' Distant Past |
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131 | (4) |
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When Did the Martian Valleys Form? |
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135 | (1) |
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136 | (2) |
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Mechanisms for Warming Early Mars |
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138 | (6) |
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Where Are the Carbonates? |
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144 | (3) |
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147 | (24) |
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Planetary Size / Magnetic Fields |
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147 | (5) |
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Ozone and Ultraviolet Radiation |
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152 | (3) |
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Availability of Nitrogen and the Importance of N2 |
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155 | (2) |
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Is Plate Tectonics Common? |
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157 | (4) |
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A Planet's Impact Environment |
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161 | (3) |
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Stabilization of Earth's Obliquity by the Moon |
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164 | (7) |
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Habitable Zones around Stars |
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171 | (24) |
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Historical Attempts to Define the Habitable Zone |
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171 | (5) |
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A More Modern Model for the Habitable Zone around the Sun |
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176 | (3) |
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Hertzsprung-Russell Diagrams and Main Sequence Stars |
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179 | (2) |
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Habitable Zones around Other Stars |
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181 | (4) |
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Problems for Planets Orbiting Early-Type Stars |
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185 | (3) |
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Problems for Planets Orbiting Late-Type Stars |
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188 | (3) |
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Further Extensions of the Habitable Zone Concept |
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191 | (1) |
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The Galactic Habitable Zone |
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192 | (3) |
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Part IV: How to Find Another Earth |
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195 | (104) |
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Indirect Detection of Planets around Other Stars |
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197 | (24) |
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198 | (1) |
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199 | (6) |
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205 | (2) |
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207 | (3) |
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The Radial Velocity Method |
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210 | (6) |
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Gravitational Microlensing |
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216 | (5) |
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Finding and Characterizing Planets by Using Transits |
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221 | (18) |
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Transits of Mercury and Venus |
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221 | (1) |
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Transits of Extrasolar ``Hot Jupiters'' |
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222 | (5) |
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Space-Based Transit Searches: CoRoT and Kepler |
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227 | (2) |
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Observing Exoplanet Atmospheres during Transits |
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229 | (4) |
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Secondary Transit Spectroscopy |
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233 | (2) |
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Characterizing Earth-Like Planets around M Stars |
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235 | (4) |
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Direct Detection of Extrasolar Planets |
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239 | (19) |
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What Wavelength Region Should We Choose? |
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240 | (5) |
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Infrared Interferometers: TPF-I and Darwin |
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245 | (3) |
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Searching for Planets at Visible Wavelengths: TPF-C |
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248 | (5) |
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The Visible Occulter: TPF-O |
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253 | (1) |
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254 | (4) |
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The Spectroscopic Search for Life |
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258 | (26) |
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259 | (1) |
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The Visible/Near-IR Region: TPF-C or -O |
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260 | (6) |
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The Thermal-IR Region: TPF-I or Darwin |
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266 | (3) |
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Looking for Life on Early Earth-Type Planets |
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269 | (2) |
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Possible False Positives for Life |
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271 | (3) |
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Polarization Measurements: Looking for the Glint of Surface Water |
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274 | (2) |
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The Holy Grail: Simultaneous Detection of O2 and Reduced Gases |
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276 | (8) |
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Prospects for the More Distant Future |
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284 | (15) |
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NASA's Life Finder Mission |
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284 | (3) |
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Using the Sun as a Gravitational Lens |
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287 | (3) |
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The Drake Equation Revisited: The Search for Extraterrestrial Intelligence |
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290 | (9) |
Notes |
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299 | (18) |
Index |
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317 | |