TPO25-R-1翻译
TPO29 R-1原文翻译
TPO 29-R-1原文翻译Characteristics of Roman Pottery 陶器的祖先罗马人在很多方面都有非凡的成就。
当你真正触摸到那时的餐具，厨房用具或是两耳细颈酒罐（在地中海区域用于运输和储存液体的大罐子，像是酒和油）的时候，就很容易能够欣赏到它的高质量了。
但是，看起来罗马器具几乎是不可能再现在纸上的，即使照片和绘画能带回那些语言。
大部分罗马的陶器是很轻的，并且摸起来非常光滑，坚硬，即使像所有的陶器一样，如果掉在硬面上就会摔碎。
一般这种陶器是由精心挑选和纯化泥土制成，在快速转轮上形成有薄壁和标准化的形状并且在窑（陶器烤炉）中烧制到能够保持永久不变的形状。
手工制作的陶器，不可避免同样设计的容器间有一些个体差异，偶尔会出现小缺陷。
但是，最吸引人眼球，立即能让人感受到的，罗马陶器最有力量的，就是持续的高质量。
这不光是作为审美考虑，也与实用性有关。
这些容器都是实心的（易碎，但不脆弱），它们舒适并且易于拿握（轻并且光滑），除此之外，由于它们坚硬有时光亮透明的表面，他们的很好的承载了液体，并且容易清洗。
此外，他们有规律和标准化的形状使得他们易于堆放。
当现在的人向人展示一个常见的罗马瓶的时候，尤其是，可以又把手拿起的，他们经常评论说这个瓶子看起来感觉起来是多么现代，他们需要去被告知说服它的真实年龄。
罗马陶器与质量一样出众的另一特点就是其巨大的数量。
当提到数量时，我们习惯于理想化的去估计一个特定生产点的生产总数，和某一个居住地区的总消费数量。
不幸的是，考古学证据的自然特性决定了每一个样本都是不同的，因此这样的数据图形是难以捉摸的。
但是，没有在这个领域工作的人会质疑罗马陶器的繁盛，特别是在地中海地区。
这种繁盛在罗马居住区是显著的，尤其是在城市地区，在这些地方，考古人员必须将陶瓷碎片进行清洗和分类，这些工作在挖掘初期的工作中占据了很大的比重。
我们只能从少量的陶器废墟中去推算“真实的”数量。
但是，有一个废墟是个例外，它代表了大部分遗址的历史消耗量，通过消耗量就可以建立起生产数据。
tpot听力25解析
TPO25listening 问题解析注：问题中红色标记词汇为解题突破点和关键词。
Section 1TPO25-L1 Conversation 11.What is the conversation mainly about? 00:09A.The student’s eligibility to graduate next semesterB.The student’s difficulties in registering for classesC. A difficult class the student must take next semesterD.Possible elective choices in the student’s degree program答案：A解析：主旨题，问的是，what’s…mainly about,男同学说的第一句我填完了毕业相关表格，但不知道下学期能否毕业。
原文如下：I’m just filling out this approval for graduation form for the Dean’s office and …I d on’t know, I hope I’ll be able to graduate next semester.2.According to the woman, why was the program’s curriculum changed? 00:45A.To attract more international students to the programB.To reflect the growing importance of international businessC.To take advantage of the expertise of new faculty membersD.To give students a stronger background in management答案：B解析：对话继续，男生说了I got confused because the way, uh, they’ve changed the requirements, so, now I’m not sure I’ll qualify to graduate next semester.紧接着，教授对这个情况进行了解释why …change.因此前面有个关键词confused because…change..原文如下：Well, when the business department changed the curriculum to include more courses in international business to dwell, because of the increasing globalization of business,3.What does the woman imply about the new departmental requirements? 00:45A.They will not affect the student’s plans for graduationB.They will not be officially approved by the department until next yearC.They will be limited to students specializing in the international businessD.They will be similar to recent changes made in other departments at the university答案：A解析：态度题，教授解释完为什么改变要求后，紧接着用make sure….3,4年级wouldn’t be affected 来安慰那个那声，并且后面紧跟着only 特别强调说明这是为了第一，二年的新生。
托福阅读tpo52R-1原文+译文+题目+答案+背景知识
TPO52阅读-1 Stream Deposit原文 (1)译文 (2)题目 (3)答案 (7)背景知识 (9)原文Stream Deposit①A large, swift stream or river can carry all sizes of particles, from clay to boulders. When the current slows down, its competence (how much it can carry) decreases and the stream deposits the largest particles in the streambed. If current velocity continues to decrease - as a flood wanes, for example - finer particles settle out on top of the large ones. Thus, a stream sorts its sediment according to size. A waning flood might deposit a layer of gravel, overlain by sand and finally topped by silt and clay. Streams also sort sediment in the downstream direction. Many mountain streams are choked with boulders and cobbles, but far downstream, their deltas are composed mainly of fine silt and clay. This downstream sorting is curious because stream velocity generally increases in the downstream direction. Competence increases with velocity, so a river should be able to transport larger particles than its tributaries carry. One explanation for downstream sorting is that abrasion wears away the boulders and cobbles to sand and silt as the sediment moves downstream over the years. Thus, only the fine sediment reaches the lower parts of most rivers.②A stream deposits its sediment in three environments: Alluvial fans and deltas form where stream gradient (angle of incline) suddenly decreases as a stream enters a flat plain, a lake, or the sea; floodplain deposits accumulate on a floodplain adjacent to the stream channel; and channel deposits form in the stream channel itself. Bars, which are elongated mounds of sediment, are transient features that form in the stream channel and on the banks. They commonly form in one year and erode the next. Rivers used for commercial navigation must be recharged frequently because bars shift from year to year. Imagine a winding stream. The water on the outside of the curve moves faster than the water on the inside. The stream erodes its outside bank because the current's inertia drives it into the outside bank. At the same time, the slower water on the inside point of the bend deposits sediment, forming a point bar. A mid-channel bar is a sandy and gravelly deposit that forms in the middle of a stream channel.③Most streams flow in a single channel. In contrast, a braided stream flows in many shallow, interconnecting channels. A braided stream forms where moresediment is supplied to a stream than it can carry. The stream dumps the excess sediment, forming mid-channel bars. The bars gradually fill a channel, forcing the stream to overflow its banks and erode new channels. As a result, a braided stream flows simultaneously in several channels and shifts back and forth across its floodplain. Braided streams are common in both deserts and glacial environments because both produce abundant sediment. A desert yields large amounts of sediment because it has little or no vegetation to prevent erosion. Glaciers grind bedrock into fine sediment, which is carried by streams flowing from the melting ice. If a steep mountain stream flows onto a flat plain, its gradient and velocity decrease sharply. As a result, it deposits most of its sediment in a fan-shaped mound called an alluvial fan. Alluvial fans are common in many arid and semiarid mountainous regions.④A stream also slows abruptly where it enters the still water of a lake or ocean. The sediment settles out to form a nearly flat landform called a delta. Part of the delta lies above water level, and the remainder lies slightly below water level. Deltas are commonly fan-shaped, resembling the Greek letter "delta" (∆). Both deltas and alluvial fans change rapidly. Sediment fills channels (waterways), which are then abandoned while new channels develop as in a braided stream. As a result, a stream feeding a delta or fan splits into many channels called distributaries. A large delta may spread out in this manner until it covers thousands of square kilometers. Most fans, however, are much smaller, covering a fraction of a square kilometer to a few square kilometers. The Mississippi River has flowed through seven different delta channels during the past 5,000 to 6,000 years. But in recent years, engineers have built great systems of levees (retaining walls) in attempts to stabilize the channels.译文溪流沉积物①一条大而湍急的小溪或河流可以承载各种大小的颗粒，从微小的粘土到巨石。
托福阅读tpo30R-1原文+译文+题目+答案+背景知识
托福阅读tpo30R-1原文+译文+题目+答案+背景知识原文 (1)译文 (4)题目 (7)答案 (16)背景知识 (17)原文Role of Play in Development①Play is easier to define with examples than with concepts. In any case, in animals it consists of leaping, running, climbing, throwing, wrestling, and other movements, either along, with objects, or with other animals. Depending on the species, play may be primarily for social interaction, exercise, or exploration. One of the problems in providing a clear definition of play is that it involves the same behaviors that take place in other circumstance--dominance, predation, competition, and real fighting. Thus, whether play occurs or not depends on the intention of the animals, and the intentions are not always clear from behaviors alone.②Play appears to be a developmental characteristic of animals withfairly sophisticated nervous systems, mainly birds and mammals. Play has been studied most extensively in primates and canids (dogs). Exactly why animals play is still a matter debated in the research literature, and the reasons may not be the same for every species that plays. Determining the functions of play is difficult because the functions may be long-term, with beneficial effects not showing up until the animal's adulthood.③Play is not without considerable costs to the individual animal. Play is usually very active, involving movement in space and, at times, noisemaking. Therefore, it results in the loss of fuel or energy that might better be used for growth or for building up fat stores in a young animal. Another potential cost of this activity is greater exposure to predators since play is attention-getting behavior. Great activities also increase the risk of injury in slipping or falling.④The benefits of play must outweigh costs, or play would not have evolved, according to Darwin' s theory. Some of the potential benefits relate directly to the healthy development of the brain and nervous system. In one research study, two groups of young rats were raised under different conditions. One group developed in an "enriched" environment, which allowed the rats to interact with other rats, play with toys, and receive maze training. The other group lived in an"impoverished" environment in individual cages in a dimly lit room with little stimulation. At the end of the experiments, the results showed that the actual weight of the brains of the impoverished rats was less than that of those raised in the enriched environment (though they were fed the same diets). Other studies have shown that greater stimulation not only affects the size of the brain but also increase the number of connections between the nerve cells. Thus, active play may provide necessary stimulation to the growth of synaptic connections in the brain, especially the cerebellum, which is responsible for motor functioning and movements.⑤Play also stimulates the development of the muscle tissues themselves and may provide the opportunities to practice those movements needed for survival. Prey species, like young deer or goats, for example, typically play by performing sudden flight movements and turns, whereas predator species, such as cats, practice stalking, pouncing, and biting.⑥Play allows a young animal to explore its environment and practice skill in comparative safety since the surrounding adults generally do not expect the young to deal with threats or predators. Play can also provide practice in social behaviors needed for courtship and mating. Learning appropriate social behaviors is especially important for species that livein groups, like young monkeys that needed to learn to control selfishness and aggression and to understand the give-and-take involved in social groups. They need to learn how to be dominant and submissive because each monkey might have to play either role in the future. Most of these things are learned in the long developmental periods that primates have, during which they engage in countless play experiences with their peers.⑦There is a danger, of course, that play may be misinterpreted or not recognized as play by others, potentially leading to aggression. This is especially true when play consists of practicing normal aggressive or predator behaviors. Thus, many species have evolved clear signals to delineate playfulness. Dogs, for example, will wag their tails, get down their front legs, and stick their behinds in the air to indicate "what follows is just for play."译文玩耍在成长中的角色①用例子比用概念更容易定义玩耍。
托福阅读TPO25-1 The Surface of Mars
Tpo25The Surface of MarsThe surface of Mars shows a wide rangeof geologic features, including huge volcanoes-the largest known in the solar system-and extensive impact cratering. Three very large volcanoes are found on the Tharsis bulge, an enormousgeologic area near Mars’s equator. Northwest of Tharsis is the largest volcano of all: Olympus Mons, with a height of 25 kilometers and measuring some 700 kilometers in diameter at its base. The three large volcanoes on the Tharsis bulge are a little smaller-a “mere” 18 kilometers high.None of these volcanoes was formed as a result of collisions between platesof the Martian crust-there is no plate motion on Mars. Instead, they are shield volcanoes — volcanoes with broad, sloping slides formed by molten rock. All four show distinctivelava channels and other flow features similar to those found on shield volcanoes on Earth. Images of the Martian surface reveal many hundreds of volcanoes. Most of the largest volcanoes are associated with the Tharsis bulge, but many smaller ones are found in the northern plains.The great height of Martian volcanoes is a directconsequence of the planet’s low surface gravity. As lava flows and spreads to form a shi eld volcano, the volcano’s eventual height depends on the new mountain’s ability to support its own weight. The lower the gravity, the lesser the weight and the greater the height of the mountain. It is no accident that Maxwell Mons on Venus and the Hawaiian shield volcanoes on Earth rise to about the same height (about 10 kilometers) above their respective bases-Earth and Venus have similar surface gravity. Mars’s surface gravity is only 40 percent that of Earth, so volcanoes rise roughly2.5 times as high. Are the Martian shield volcanoes still active? Scientists have no direct evidence for recent or ongoing eruptions, but if these volcanoes were active as recently as 100 million years ago (an estimate of the time of last eruption based on the extent of impact cratering on their slopes), some of them may still be at least intermittently lions of years, though, may pass between eruptions.Another prominent feature of Mars’s surface is cratering. The Mariner spacecraft found that the surface of Mars, as well as that of its two moons, is pitted with impact craters formed by meteoroids falling in from space. As on our Moon, the smaller craters are often filled with surface matter-mostly dust-confirming that Mars is a dry desert world. However, Martian craters get filled in considerablyfaster than their lunar counterparts. On the Moon, ancient craters less than 100 meters across (corresponding to depths of about 20 meters) have been obliterated, primarily by meteoritic erosion. On Mars, there are relatively few craters less than 5 kilometers in diameter. The Martian atmosphere is an efficient erosive agent, with Martian winds transporting dust from place to place and erasing surface features much faster than meteoritic impacts alone can obliterate them.As on the Moon, the extent of large impact cratering (i.e. craters too big to have been filled in by erosion since they were formed) servesas an age indicator for the Martian surface. Age estimates ranging from four billion years for Mars’s southern highla nds to a few hundred million years in the youngest volcanic areas were obtained in this way.The detailed appearance of Martian impact craters provides an important piece of information aboutconditions just below the planet’s surface. Martian craters are surrounded by ejecta (debris formed as aresult of an impact) that looks quite different from its lunar counterparts. A comparison ofthe Copernicuscrater on the Moon with the (fairly typical) crater Yuty on Mars demonstrates the differences. The ejectasurrounding the lunar crater is just what one would expect from an explosion ejecting a large volume of dust,soil, and boulders. However, the ejecta on Mars gives the distinct impression of a liquid that has splashed orflowed out of crater. Geologists think that this fluidized ejecta crater indicates that a layer of permafrost, orwater ice, lies just a few meters under the surface. Explosive impacts heated and liquefied the ice, resultingin the fluid appearance of the ejecta.Paragraph 1:The surface of Mars shows a wide rangeof geologic features, including huge volcanoes-the largest known in the solar system-and extensive impact cratering. Three very large volcanoes are found on the Tharsis bulge, ant of Tharsis is the largest volcano of all: Olympus Mons, with a height of 25 kilometers and measuring some 700 kilometers in diameter at its base. The three large volcanoes on the Tharsis bulge are a little smaller-a “mere” 18 kilometers high.1. The wo○ Important○ Extremely large○ Highly unusual○ Active2. According to paragraph 1, Olympus Mons differs from volcanoes on the Tharsis bulge in that Olympus Mons○ Has more complex geologic features○ Shows less impact cratering○ Is taller○ Was formed at a later timeParagraph 2:None of these volcanoes was formed as a result of collisions between platesof the Martian crust-there is no plate motion on Mars. Instead, they are shield volcanoes-volcanoes with broad, sloping slides formed by molten rock. All four showreveal many hundreds of volcanoes. Most of the largest volcanoes are associated with the Tharsis bulge, but many smaller ones are found in the northern plains.3. meaning to○ Deep○Complex○ Characteristic○ Ancient4. According to paragraphs 1 and 2, which of the following is NOT true of the shield volcanoes on the Tharsis bulge?○ They have broad, sloping sides.○ They are smaller than the largest volcano on Mars.○ They have channels that resemble the lava channels of volcanoes on Earth.○ They are over 25 kilometers tall.Paragraph 3:The great height of Martian volcanoes is a direct consequence of the planet’s low surfacegravity. As lava flows and spreads to form a shield volcano, the volcano’s eventual height depends on thenew mountain’s ability to support its own weight. The lower the gravity, the lesser the weight and the greaterthe height of the mountain. It is no accident that Maxwell Mons on Venus and the Hawaiian shield volcanoeson Earth rise to about the same height (about 10 kilometers) above their respective bases-Earth and Venus5. n the passage is closest in meaning to○ Typically○ Frequently○ Actually○ Approximately6. In paragraph 3, why does the author compare Maxwell Mons on Venus to the Hawaiian shieldvolcanoes on Earth?○ To help explain the relationship between surface gravity and volcano height○To explain why Mars’s surface gravity is only 40 percent of Earth’s○ To point out differences between the surface gravity of Earth and the surface gravity of Venus○ To argue that there are more similarities than differences between volcanoes on different planets7. Which of the sentences below best expresses the essential information in the highlighted sentence inthe passage? Incorrect choices change the meaning in important ways or leave out essential information.○ Although direct evidence of recent eruptions is lacking, scientists believe that these volcanoes wereactive as recently as 100 million years ago.○ Scientists estimate that volcanoes active more recently than 100 years ago will still have extensiveimpact cratering on their slopes.○ If, as some evidence suggests, these volcanoes erupted as recently as 100 million years ago, theymay continue to be intermittently active.○Although these volcanoes were active as recently as 100 million years ago, there is no directevidence of recent or ongoing eruptions.Paragraph 4:Another prominent feature of Mars’s surface is cratering. The Mariner spacecraft found that the surface of Mars, as well as that of its two moons, is pitted with impact craters formed by meteoroids falling in from space. As on our Moon, the smaller craters are often filled with surface matter-mostly dust-lunar counterparts. On the Moon, ancient craters less than 100 meters across (corresponding to depths of about 20 meters) have been obliterated, primarily by meteoritic erosion. On Mars, there are relatively few craters less than 5 kilometers in diameter. The Martian atmosphere is an efficient erosive agent, with Martian winds transporting dust from place to place and erasing surface features much faster than meteoritic impacts alone can obliterate them.8.○ Frequently○ Significantly○ Clearly○ Surprisingly9. According to paragraph 4, what is demonstrated by the fact that craters fill in much faster on Mars than on the Moon?○ Erosion from meteoritic impacts takes place more quickly on Mars than on the Moon.○ There is more dust on Mars than on the Moon.○ The surface of Mars is a dry desert.○ Wind is a powerful eroding force on Mars.10. In paragraph 4, why does the author point out that Mars has few ancient craters that are less than 5 kilometers in diameter?○ To explain why scientists believe that the surface matter filling Martian craters is mostly dust○ To explain why scientists believe that the impact craters on Mars were created by meteoroids○ To support the claim that the Martian atmosphere is an efficient erosive agent○ To argue that Mars experienced fewer ancient impacts than the Moon didParagraph 5:As on the Moon, the extent of large impact cratering (i.e. craters too big to have been filled in by erosion since they were formed) servesas an age indicator for the Martian surface. Age estimates ranging from four billion years for Mars’s southern highlands to a few hundred million years in the youngest volcanic areas were obtained in this way.11. According to paragraph 5, what have scientists been able to determine from studies of large impact cratering on Mars?○ Some Martian volcanoes are much older than was once thought.○The age of Mars’s surface can vary from area to area.○ Large impact craters are not reliable indicators of age in areas with high volcanic activity.○ Some areas of the Martian surface appear to be older than they actually are.The detailed appearance of Martian impact craters provides an important piece of information about conditions just below the planet’s surface. Martian craters are surrounded by ejecta (debris formed as a result of an impact) that looks quite different from its lunar counterparts. A comparison ofthe Copernicus crater on the Moon with the (fairly typical) crater Yuty on Mars demonstrates the differences. The ejecta surrounding the lunar crater is just what one would expect from an explosion ejecting a large volume of dust, soil, and boulders. ■However, the ejecta on Mars gives the distinct impression o f a liquid that has splashed or flowed out of crater. ■Geologists think that this fluidized ejecta crater indicates that a layer of permafrost, or water ice, lies just a few meters under the surface. ■Explosive impacts heated and liquefied the ice, resulti ng in the fluid appearance of the ejecta. ■12. According to paragraph 6, the ejecta of Mars’s crater Yuty differs from the ejecta of the Moon’s Copernicus crater in that the ejecta of the Yuty crater○ Has now become part of a permafrost layer○ Contains a large volume of dust, soil and boulders○ Suggests that liquid once came out of the surface at the crater site○ Was thrown a comparatively long distance from the center of the crater13. Look at the four squares【■】that indicate where the following sentence could be added to the passage.This surface feature has led to speculation about what may lie under Mars’s surface.Where would the sentence best fit? Click on a square to add the sentence to the passage.14. Directions: An introductory sentence for a brief summary of the passage is provided below. Complete the summary by selecting the THREE answer choices that express the most important ideas in the passage. Some sentences do not belong in the summary because they express ideas that are not presented in the passage or are minor ideas in the passage. This question is worth 2 points.Drag your answer choices to the spaces where they belong. To remove an answer choice, click on it. To review the passage, click VIEW NEXT.Volcanoes and impact craters are major features of Martian geology.Answer Choices●●●○Plate motion on Mars, once considered to have played no role in shaping the planet’s surface, is now seen as being directly associated with the planet’s earliest volcanoes.○Mars has shield volcanoes, some of which are extremely tall because of the planet’s low surface gravity.○ Although the erosive power of the Martian atmosphere ensures that Mars has fewer craters than the Moon does, impact cr aters are prominent on Mars’ s surface.○Scientists cannot yet reliably estimate the age of the Martian surfacebecause there has been too much erosion of it.○Scientists have been surprised to discover that conditions just below the surface of Mars are very similar to conditions just below the surface of the Moon○Studies of crater ejecta have revealed the possibility of a layer of permafrost below the surface of Mars.参考答案：1.22. 33. 34. 45.46. 17. 38.29. 410. 311. 212. 313. 214. Mars has shield volcanoes, ... Although the erosive power... Studies of crater ejecta have...。
新托福TPO25阅读原文及译文(一)
新托福TPO25阅读原文(一)：The surface of MarsTPO25-1：The surface of MarsThe surface of Mars shows a wide range of geologic features, including huge volcanoes-the largest known in the solar system-and extensive impact cratering. Three very large volcanoes are found on the Tharsis bulge, an enormous geologic area near Mars’s equator. Northwest of Tharsis is the largest volcano of all: Olympus Mons, with a height of 25 kilometers and measuring some 700 kilometers in diameter at its base. The three large volcanoes on the Tharsis bulge are a little smaller-a “mere”18 kilometers high.None of these volcanoes was formed as a result of collisions between plates of the Martian crust-there is no plate motion on Mars. Instead, they are shield volcanoes —volcanoes with broad, sloping slides formed by molten rock. All four show distinctive lava channels and other flow features similar to those found on shield volcanoes on Earth. Images of the Martian surface reveal many hundreds of volcanoes. Most of the largest volcanoes are associated with the Tharsis bulge, but many smaller ones are found in the northern plains.The great height of Martian volcanoes is a direct consequence of the planet’s low surfac e gravity. As lava flows and spreads to form a shield volcano, the volcano’s eventual height depends on the new mountain’s ability to support its own weight. The lower the gravity, the lesser the weight and the greater the height of the mountain. It is no accident that Maxwell Mons on Venus and the Hawaiian shield volcanoes on Earth rise to about the same height (about 10 kilometers) above their respective bases-Earth and Venus have similar surface gravity. Mars’s surface gravity is only 40 percent that of Earth, so volcanoes rise roughly2.5 times as high. Are the Martian shield volcanoes still active? Scientists have no direct evidence for recent or ongoing eruptions, but if these volcanoes were active as recently as 100 million years ago (an estimate of the time of last eruption based on the extent of impact cratering on their slopes), some of them may still be at least intermittently active. Millions of years, though, may pass between eruptions.Another prominent feature of Mars’s surface is cratering. T he Mariner spacecraft found that the surface of Mars, as well as that of its two moons, is pitted with impact craters formed by meteoroids falling in from space. As on our Moon, the smaller craters are often filled with surface matter-mostly dust-confirming that Mars is a dry desert world. However, Martian craters get filled in considerably faster than their lunar counterparts. On the Moon, ancient craters less than 100 meters across (corresponding to depths of about 20 meters) have been obliterated, primarily by meteoritic erosion. On Mars, there are relatively few craters less than 5 kilometers in diameter. The Martian atmosphere is an efficient erosive agent, with Martian winds transporting dust from place to place and erasing surface features much faster than meteoritic impacts alone can obliterate them.As on the Moon, the extent of large impact cratering (i.e. craters too big to have been filled in by erosion since they were formed) serves as an age indicator for the Martian surface. Age estimates ran ging from four billion years for Mars’s southern highlands to a few hundred million years in the youngest volcanic areas were obtained in this way.The detailed appearance of Martian impact craters provides an important piece of information about conditi ons just below the planet’s surface. Martian craters are surrounded by ejecta (debris formed as a result of an impact) that looks quite different from its lunar counterparts. A comparison of the Copernicus crater on the Moon with the (fairly typical) crater Yuty on Mars demonstrates the differences. The ejecta surrounding the lunar crater is just what one would expect from an explosion ejecting a large volume of dust, soil, and boulders. However, the ejecta on Mars gives the distinct impression of a liquid that has splashed or flowed out of crater. Geologists think that this fluidized ejecta crater indicates that a layer of permafrost, or water ice, lies just a few meters under the surface. Explosive impacts heated and liquefied the ice, resulting in the fluid appearance of the ejecta.TPO25-1译文：火星表面火星表面展示了很多种地理特征，包括巨大的火山——太阳系中已知的最大火山——以及覆盖范围很广的陨石坑。
托福TPO25 section1 翻译
TPO25 Coversation1ProfessorHi, Mark. What can I do for you?你好，Mark. 我能为你做点什么？StudentI am just filling out this approval for graduation form for the dean's office, and I don't know, I hope I will be able to graduate next semester.我正在填写要交给系主任办公室的毕业批准表格，我不知道会不会批准，希望下个学期我能够毕业。
ProfessorWell, as long as you've met the departmental requirements and you submit the form on time, you shouldn't have any problem. Make sure you include all the classes you will have taken for your degree in finance and the electives too.只要你满足院系里的毕业要求然后按时提交表格，你就应该没有问题。
请确认你把所有上过的金融专业的课都算在内还有那些选修课。
StudentYeah, but as I look over the form, I got confused because of the way, um…they've changed the requirements. So now I am not sure I will be qualified to graduate next semester. I know I would, before, under the old requirements.是的，但是看了这份表格之后，我有些困惑，因为他们改变了要求。
托福听力必背长难句
01:12-01:17
And then before we decide to include a book in the sale, we review itscirculationhistory again,which can take a while.We've got a lot of books in storage.
Tpo34-l4
00:49-00:56
But eventually, moving over to the right side there, interest begins tofadeand the growth and saleslevels off.
03:09-03:19
And as a market analyst, you could say that with Kind of Blue, he wjumping
00:38-00:45
We have government recycling programs for materials like plastics, glass and metal,yetwidespread solutions for organic waste materialshaven,t really beenaddressedin the United States.
Tpo25-l3
0139-45
The rosetta stone was remarkable because as I said, on it, was the same text in three differentalphabets.
Tpo33-l4
0113-22
As we have said before, the main point of therenaissancewas to revive the genius of the ancient Greeks and Romans, which is why designers of renaissance gardens designed them as the ancient Romanswould have designed them, or at least as they imagined the ancient Romans would have designed them.
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TPO25-R-1翻译
翻译：Jelly
校对：大寶大頭
火星的表面
火星的表面有各种的地质特征，包括在太阳系中已知最巨型火山和大量的陨石坑。
三个非常巨型的火山发现在萨希斯凸出地区，这是一个靠近火星赤道的巨大地质区域。
萨希斯的西北部是最大的火山——奥林巴斯山，高度是25千米以及底部直径为700千米。
在萨西斯凸出地区的其他三个火山相对小一些，仅有18千米高。
因为火星上面没有板块运动，没有一个火山的成因是由于火星外壳板块挤压形成的。
反而，他们都是盾形火山，这些火山由大面积熔岩有倾斜度地滑动形成的。
这四座火山都拥有与地球上的盾形火山相同的熔岩通道和其他一些流体特征。
图片显示火星表面显露出来的成百上千的火山，其中大多数巨型火山都在萨西斯凸出地区，相对小一些的在北部平原上。
火星上火山的高度是由这个行星的低地心引力导致的。
由于熔岩的流动和蔓延形成了盾形火山，这个火山的最终高度决定于它支撑整个重量的能力。
地心引力越低，这个山的的重力就越小，高度就越高。
毫无疑问，因为地球和金星的地表地心引力是一样的，金星上的麦斯威尔山和地球上夏威夷的盾形火山在他们各自的基础上上升至相同的高度（大约10千米）。
火星的地表引力只有地球的40%，因此火山上升高度粗略来看是2.5倍。
火星上的盾形火山还是活火山吗？科学家没有直接证据表明有近期或者不间断的火山喷发迹象，但是如果这些火山最近一次活动是在10千万年前（时间上的估算是根据斜坡上的陨石坑的范围决定的），大部分至少可能还在间接性运动。
虽然爆发间隙会是千万年。
火星表面的另一个突出特征就是陨石坑。
宇宙飞船上的宇航员和两颗人造卫星发现，火星表面是由于太空中的流星体跌落所造成的陨石坑。
正如在我们的月球上面，相对小的陨石
坑大部分都是被尘埃充满了表面，从而确定火星也是一个干旱的沙漠世界。
然而，火星上的陨石坑被填满速度比月球上的快非常多。
在月球上，主要是由陨石腐蚀，年代久远的陨石坑直径小于100米（相对深度大约20米）都已经被堵塞了。
在火星上，相对少的陨石坑直径小于5千米。
（造成这种情况的主要原因是）火星上大气层是一个高效的腐蚀中介，风会将尘埃从一个地方转到另外一个地方并且它消除地表特征比单独因为陨石撞击快得多。
因为在月球上，巨型陨石坑的范围（至形成以来陨石坑太大以至于不能被腐蚀填满）作为一个火星表面年龄的指示器。
根据这种方法，年龄范围的估算从火星南部高地的40亿年到最年轻的火山地区的十几千万年不等。
火星陨石坑的细节表象提供了一条关于星球地表下方条件的重要信息。
火星陨石坑被喷出物（由于撞击产生的碎片）所包围，看起来和月球上的不太一样。
在月球上的哥白尼陨石坑和在火星上相对有代表性的Yuty陨石坑证明了这种差异。
月球陨石坑周围的喷出物是一次爆炸喷射出来的大量的尘埃，土壤和岩石形成的。
然而，火星上的喷出物给了流体一个明显的形象，是喷散或者流出陨石坑的。
地质学家认为这种流态化的喷出物陨石坑证明了永久冻土带或冰水都只是在地表下几米而已。
爆炸性地撞击加热和液化了冰，造成喷出物的液态状。