2. 外语
  3. Surface Fluids on Venus and Earth P1: When astronomers first pointed their rudimentary telescopes at Venus, they saw a world shr

Surface Fluids on Venus and Earth P1: When astronomers first pointed their rudimentary telescopes at Venus, they saw a world shr

admin2018-10-18  51
问题 Surface Fluids on Venus and Earth
P1: When astronomers first pointed their rudimentary telescopes at Venus, they saw a world shrouded in clouds. Here on Earth, clouds mean water, so early astronomers imagined a tropical world with constant rainfall. The truth, of course, is that the hydrological state on Venus is quite different from that of Earth. The hydrologic cycle describes the continuous movement of liquid above, on, and below the surface of a planet. These movements derive their energy from the Sun and the gravitational forces of the planet itself, and in turn redistribute energy around the globe through atmospheric circulation. As fluids interact with surface materials, water molecules move particles repeatedly through solid, liquid, and gaseous phases or react chemically with them to modify and produce materials. On a solid planet with a hydrosphere and an atmosphere, only a tiny fraction of the planetary mass flows as surface fluids. Yet, the movements of these fluids can drastically alter a planet.
P2: Imagine Venus a long time ago. The planet is nearly identical to the Earth in size, mass, composition and distance from the Sun. However, it lacks any sign of a hydrologic system—there are no streams, lakes, oceans, or glaciers. It begins like the Earth with global oceans, carbon dioxide dissolved in the oceans, and carbonate rocks forming at the bottoms of the oceans. But because Venus is just a tiny bit smaller than the Earth, it has less radioactive heat sources inside. Thus, at some time in the distant past, perhaps only 500 million to 1 billion years ago, Venus may have run out of enough internal heat to continue to drive the tectonic activity. Alternatively, because Venus is a little closer to the Sun, we would expect that the original temperature of Venus should have been a little warmer than that of the early Earth. The slightly elevated temperature puts a bit more water in the oceans and atmosphere and a bit less in the rocks. This makes the rocks harder since water serves as a lubricant for the plate tectonic process. Either way, tectonic activity begins to slow down. Because Venus receives more heat from the Sun, water released from the interior evaporated and rose to the upper atmosphere, where the Sun’s ultraviolet rays broke the molecules apart. Much of the freed hydrogen escaped into space, and Venus lost its water. Without water, Venus became less and less like Earth and kept an atmosphere filled with carbon dioxide. On Earth, liquid water removes carbon dioxide from the atmosphere and combines it with calcium, through rock weathering, to form carbonate sedimentary rocks. Without liquid water to remove carbon from the atmosphere, prohibiting the formation of carbonate minerals, the level of carbon dioxide in the atmosphere of Venus remains high.
P3: Like Venus, Earth is large enough to be geologically active and for its gravitational field to hold an atmosphere. But fortunately, being further away, it has less heating from the sun and allows water to exist as a liquid, a solid, and a gas. Water is thus extremely mobile and moves rapidly over the planet in a continuous hydrologic cycle. Driven by energy from the sun, water is constantly being cycled from the ocean, through the atmosphere, and ultimately back to the oceans. As a result, Earth’s surface has been continually changed and eroded into delicate systems of river valleys—a remarkable contrast to the surfaces of other planetary bodies where impact craters dominate. Other geologic changes occur when the gases in the atmosphere or water react with rocks at the surface to form new chemical components with different properties. Weathering breaks down rocks into gravel, sand, and sediment, and is an important source of key nutrients such as calcium and sulfur. Estimates indicate that, on average, Earth’s surface weathers at a rate of about 0.5 millimeter per year. Actual rates may be much higher at specific locations and may have been accelerated by human activities. However, none of these would have happened if our planet had spun a little further from or nearer to the sun. Because liquid water was present, self-replicating molecules of carbon, hydrogen, and oxygen developed life early in Earth’s history and have rapidly modified its surface, blanketing huge parts of the continents with greenery.
P2: Imagine Venus a long time ago. The planet is nearly identical to the Earth in size, mass, composition and distance from the Sun. ■ However, it lacks any sign of a hydrologic system—there are no streams, lakes, oceans, or glaciers.■ It begins like the Earth with global oceans, carbon dioxide dissolved in the oceans, and carbonate rocks forming at the bottoms of the oceans. ■But because Venus is just a tiny bit smaller than the Earth, it has less radioactive heat sources inside. Thus, at some time in the distant past, perhaps only 500 million to 1 billion years ago, Venus may have run out of enough internal heat to continue to drive the tectonic activity. Alternatively, because Venus is a little closer to the Sun, we would expect that the original temperature of Venus should have been a little warmer than that of the early Earth. The slightly elevated temperature puts a bit more water in the oceans and atmosphere and a bit less in the rocks. This makes the rocks harder since water serves as a lubricant for the plate tectonic process. Either way, tectonic activity begins to slow down. Because Venus receives more heat from the Sun, water released from the interior evaporated and rose to the upper atmosphere, where the Sun’s ultraviolet rays broke the molecules apart. ■ Much of the freed hydrogen escaped into space, and Venus lost its water. Without water, Venus became less and less like Earth and kept an atmosphere filled with carbon dioxide. On Earth, liquid water removes carbon dioxide from the atmosphere and combines it with calcium, through rock weathering, to form carbonate sedimentary rocks. Without liquid water to remove carbon from the atmosphere, prohibiting the formation of carbonate minerals, the level of carbon dioxide in the atmosphere of Venus remains high.
According to paragraph 3, Earth’s surface is different from the surfaces of many other planetary bodies in which of the following ways?
选项 A、It is more strongly marked by river valleys and erosion.
B、It is more geologically active.
C、It is covered by impact craters.
D、It has an atmosphere.
答案A
解析 【事实信息题】破折号后提到“remarkable contrast to the surfaces of other planetary bodies where impact craters dominate”说明此处谈到了与其他星球的差异，破折号解释说明的正是前面的“river valleys”，因此答案为A。
转载请注明原文地址:https://kaotiyun.com/show/QwfO777K
0

托福（TOEFL）

相关试题推荐
随机试题
最新回复(0)