When Extrasolar Planets Transit Their Parent Stars
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小学下册英语第1单元测验卷(有答案)考试时间:90分钟(总分:110)A卷一、综合题(共计100题共100分)1. 填空题:My brother loves to play __________. (足球)2. 听力题:We go _____ (fishing/camping) every summer.3. 填空题:The ________ (生态影响因素) shape ecosystems.4. 填空题:My toy _____ can fly high.5. 听力题:The chemical formula for cyclohexane is ______.6. 选择题:What is the name of the famous character who lives in a shoe?A. Old Mother HubbardB. The Old Woman Who Lived in a ShoeC. CinderellaD. Goldilocks7. 听力题:You can find _______ in a garden or park.8. 填空题:I enjoy making ______ (美食) for my friends during gatherings.9. 听力题:A _______ can measure the amount of energy consumed by an appliance over time.10. 填空题:The __________ (历史的传承角色) connect generations.What is the name of the famous tower in Paris?A. Eiffel TowerB. Leaning Tower of PisaC. Burj KhalifaD. Space Needle答案: A12. 填空题:The ________ was a major turning point in the history of Europe.13. 填空题:The __________ (历史的纪录片) offer visual insights into the past.14. 听力题:Plants absorb carbon dioxide through their ______.15. 选择题:What do we call the time when the sun rises?A. SunriseB. SunsetC. DuskD. Dawn答案: A16. 听力题:Carbon dioxide is produced when we _______.17. 听力题:I have ___ (four/five) friends at school.18. ts are adapted to ______ (高海拔) environments. 填空题:Some pla19. 选择题:What is 20 divided by 5?A. 2B. 4C. 5D. 6答案:B20. 填空题:A sunflower turns towards the _____.My grandma makes the best __________ (甜点).22. 填空题:I like to visit ______ during summer break.23. 选择题:What is the opposite of hot?A. WarmB. CoolC. ColdD. Mild答案:C24. 听力题:The ______ helps make important decisions.25. 选择题:What is the capital city of the United Kingdom?A. ManchesterB. LondonC. EdinburghD. Cardiff答案: B26. 选择题:What do you call a large, slow-moving animal with a shell?A. TortoiseB. TurtleC. SnailD. Armadillo答案:A27. 选择题:What is the name of the fairy tale character who had a magic mirror?A. CinderellaB. Snow WhiteC. RapunzelD. Belle28. 听力题:My sister is ______ to a party this weekend. (going)29. 填空题:I have a pet ______ (兔子) named Fluffy. It is very soft and loves to be ______ (抚摸).What do we call the process of a liquid turning into a gas?A. EvaporationB. CondensationC. FreezingD. Melting答案: A31. 选择题:What do we call the water cycle's process of water vapor turning into liquid?A. EvaporationB. CondensationC. PrecipitationD. Collection答案: B32. 选择题:What is the opposite of "fast"?A. QuickB. SlowC. RapidD. Speedy答案:B33. 填空题:The _______ (虎) is a powerful hunter.34. 选择题:What do we call the process of cooking food using steam?A. BoilingB. SteamingC. FryingD. Baking答案:B35. 选择题:Which planet is known as the "Blue Planet"?A. EarthB. MarsC. VenusD. Neptune36. 填空题:The parrot has bright _________. (羽毛)The _______ of a plant can be very long.38. 填空题:_____ (花卉销售) supports local economies.39. 选择题:What term describes the shape of the orbit of planets?A. CircularB. EllipticalC. LinearD. Irregular40. 填空题:My ________ (玩具名称) comes with a set of stickers.41. 选择题:What is the name of the famous Scottish lake said to be home to a monster?A. Loch NessB. Lake SuperiorC. Lake TahoeD. Lake Victoria答案:A42. 选择题:What do we call the area of land near the sea?A. CoastB. DesertC. ForestD. Mountain43. 听力题:The Earth's surface is constantly ______ due to natural forces.44. 听力题:We have a _____ (庆典) for the festival.45. 听力题:The sky is _____ (blue/green) today.46. 选择题:What is the name of the fairy tale character who lost her glass slipper?a. Snow Whiteb. Cinderellac. Sleeping Beautyd. Rapunzel答案:B47. 听力题:A __________ is a geological feature that can impact agricultural practices.48. 听力题:The color of phenolphthalein changes in acidic and basic solutions, indicating ______.49. 听力题:My sister loves to ________.50. 听力题:I like _____ (to run/to walk).51. 选择题:What is the name of the tree that produces acorns?A. PineB. OakC. MapleD. Birch答案:B52. 选择题:What do you call the process of creating a new plant from a cutting?A. GraftingB. CloningC. PropagationD. All of the above53. 选择题:What do we call a person who studies animals?A. BiologistB. ZoologistC. BotanistD. Ecologist54. 填空题:The first successful heart transplant was performed in ______ (20世纪).55. 填空题:I love to go ________ (露营) in the summer.56. 填空题:I like to listen to ______ (故事) before I go to sleep.The process of oxidation involves the ______ of electrons.58. 选择题:What is the name of the famous artist known for his works in the Renaissance?A. Leonardo da VinciB. Vincent van GoghC. Pablo PicassoD. Claude Monet答案: A59. 选择题:What do you call a baby kangaroo?A. JoeyB. CubC. CalfD. Kit答案:A60. 听力题:Chemical changes often involve the formation of _____ or new substances.61. 听力题:A __________ is a natural resource that can be recycled.62. 选择题:How many days are in February during a leap year?a. 28b. 29c. 30d. 31答案:B63. 听力题:The ________ (dog) is barking loudly.64. 填空题:He is a _____ (评论家) who reviews films.65. 填空题:I created a _________ (玩具动物园) with all my stuffed animals.66. 填空题:There are many _______ (昆虫) in the garden.A ______ (植物的保育措施) can protect vulnerable species.68. 选择题:Which animal is known as the "king of the jungle"?A. ElephantB. LionC. TigerD. Bear答案:B69. 填空题:I can enjoy playful activities with my ________ (玩具类型).70. 填空题:At recess, we play ________ (游戏) on the playground. I love to play ________ (足球) with my classmates.71. 填空题:The __________ is a major geographical feature in Europe. (阿尔卑斯山)72. 填空题:A _____ (城市绿化) initiative can improve living conditions.73. 听力题:They are ___ (singing/playing) together.74. 选择题:What is the name of the famous river in Egypt?A. AmazonB. MississippiC. NileD. Yangtze75. 填空题:Certain plants are known for their ______ (药用性质).76. 听力题:The _____ (hedgehog) is spiky.77. 听力题:The process of oxidation involves __________ losing electrons.78. 选择题:What do we call a person who studies the weather?A. ClimatologistB. MeteorologistC. EnvironmentalistD. Geologist79. 选择题:What is the capital of Mongolia?A. UlaanbaatarB. HohhotC. ErdenetD. Darkhan答案:A. Ulaanbaatar80. 填空题:The chef, ______ (厨师), teaches cooking classes.81. 听力题:A ______ is a cold-blooded animal that lays eggs.82. 听力题:A __________ is an area of land that is covered with trees.83. 填空题:The anteater's long snout is perfect for eating ______ (蚂蚁).84. 填空题:The ________ was a famous naval battle during World War II.85. 选择题:Which of these animals can swim?A. LionB. WhaleC. HorseD. Monkey86. 填空题:My sister loves to read ____.87. 听力题:The chemical properties of an element depend on its ______.88. 听力题:A __________ is a low area that collects water.89. 填空题:My favorite superhero _________ (玩偶) has a cool _________ (披风).90. 填空题:My __________ (玩具名) is made of __________ (材料).91. 听力题:My favorite sport is _____ (篮球).92. 选择题:What do you wear on your feet?A. HatB. GlovesC. ShoesD. Scarf93. 听力题:The snow is _______ (white).94. 听力题:The chemical symbol for cesium is _______.95. 选择题:What do we call a person who repairs cars?A. AccountantB. MechanicC. ArchitectD. Chef答案:B96. 听力题:A chemical that can cause a reaction to occur is called a ______.97. 听力题:It is ___ (raining/sunny) outside.98. 选择题:What do we call the study of the earth's physical structure?A. GeographyB. GeologyC. EcologyD. Astronomy答案: B99. 选择题:What do we call a story that teaches a moral lesson?A. FableB. MythC. LegendD. Folklore答案: A100. 填空题:I like to ride my ______ (自行车) through the neighborhood with my friends.。
高二英语天文辨析单选题40题1. Scientists have discovered that Mars has a much thinner atmosphere compared to Earth. Which of the following is a major consequence of this?A. It has a much weaker gravitational pullB. It has more extreme temperature variationsC. It has a shorter orbital periodD. It has no seasons答案解析:B。
首先分析A选项,行星的引力主要取决于其质量等因素,而不是大气厚度,所以A错误。
B选项,火星大气稀薄,不能很好地保存热量,导致昼夜和季节的温度变化非常极端,这是火星大气稀薄的一个重要结果,所以B正确。
C选项,火星的轨道周期是由其与太阳的距离等因素决定的,和大气厚度无关,C错误。
D选项,火星是有季节的,大气稀薄并不意味着没有季节,D错误。
2. Jupiter is known for its massive size. Which of the following statements about Jupiter's size is correct?A. Its diameter is about ten times that of EarthB. Its volume is exactly one thousand times that of EarthC. Its surface area is twice as large as all the other planets combinedD. Its mass is so large that it affects the orbits of all the inner planets答案解析:A。
托福阅读真题第231篇TheOriginofEarth’sAtmosphere(答案文章最后)The Origin of Earth’s AtmosphereParagraph 1:In order to understand the origin of Earth's atmosphere, we must go back to the earliest days of the solar system, before the planets themselves were formed from a disk of rocky material spinning around the young Sun. This material gradually coalesced into lumps called planetesimals as gravity and chance smashed smaller pieces together, a chaotic and violent process that became more so as planetesimals grew in size and gravitational pull. Within each orbit, collisions between planetesimals generated immense heat and energy. How violent these processes were is suggested by the odd tilt and spin of many of the planets, which indicate that each of the planets was, like a billiard ball, struck at some stage by another large body of some kind. Visual evidence of these processes can be seen by looking at the Moon. Because the Moon has no atmosphere, its surface is not subject to erosion, so it retains the marks of its early history. Its face is deeply scarred by millions of meteoric impacts, as you can see on a clear night with a pair of binoculars. The early Earth did not have much of an atmosphere. Before it grew to full size, its gravitational pull was insufficient to prevent gases from drifting off into space, while the solar wind (the great stream of atomic particles emitted from the Sun) had already driven away much of the gaseous material from the inner orbits of the solar system. So we must imagine the early Earth as a mixture of rocky materials, metals, and trapped gases, subject to constant bombardment by smaller planetesimals and without much of an atmosphere.1. The word chaotic in the passage is closest in meaning toO rapidO disorganizedO intenseO long-lasting2. All of the following are true of the planetesimals mentioned in paragraph 1 EXCEPT:O They were formed of rocky material spinning around the early Sun.O They collided violently with each other.O They gradually grew in size.O They lost their atmospheres as they were hit by larger bodies.3. The author discusses the Moon in paragraph 1 in order toO help explain why Earth had fewer meteoric impacts than other planets in the solar systemO show why it is difficult to understand how the first planetary atmospheres developedO help explain the processes that took place in the formation of large planetary bodies in the solar systemO illustrate why the Moon's spin and tilt are unique among other planetary bodies in the solar systemParagraph 2:As it began to reach full size, Earth heated up, partly because of collisions with other planetesimals and partly because of increasing internal pressures as it grew in size. In addition, the early Earth contained abundant radioactive materials, also a source of heat. As Earth heated up, its interior melted. Within the molten interior, under the influence of gravity, different elements were sorted out by density. By about 40 million years after the formation of the solar system, most of theheavier metallic elements in the early Earth, such as iron and nickel, had sunk through the hot sludge to the center, giving Earth a core dominated by iron. This metallic core gives Earth its characteristic magnetic field, which has played an extremely important role in the history of our planet.4. Paragraph 2 answers which of the following questions about early Earth?O What caused materials on Earth to become radioactive?O What percentage of Earth's core was nickel?O What internal pressures caused Earth to heat up as it grew in size?O What caused Earth's magnetic field?5. According to paragraph 2, Earth's core is mostly iron because, compared to most other elements on early Earth, iron O was denserO melted more easilyO was more radioactiveO was more plentifulParagraph 3:As heavy materials headed for the center of Earth, lighter silicates (such as the mineral quartz) drifted upward. The denser silicates formed Earth's mantle, a region almost 3,000 kilometers thick between the core and the crust. With the help of bombardment by comets, whose many impacts scarred and heated Earth's surface, the lightest silicates rose to Earth's surface, where they cooled more rapidly than the better-insulated materials in Earth's interior.Paragraph 4:These lighter materials, such as the rocks we call granites, formed a layer of continental crust about 35 kilometers thick. Relative to Earth as a whole, this is as thin as an eggshell. Seafloor crust is even thinner, at about 7 kilometers;thus, even continental crust reaches only about 1/200th of the way to Earth's core. Much of the early continental crust has remained on Earth's surface to the present day.6. Select the TWO answer choices that, according to paragraph 3 and 4, indicate true statements about Earth's formation.To obtain credit, you must select TWO answer choices.O Comets hitting Earth helped the lightest silicates to reach Earth's surface.O Silicates such as mineral quartz drifted downward and mixed with denser materials as they reached Earth's core.O When Earth's mantle became approximately 3,000 kilometers thick, the heaviest materials in it began to cool.O Lighter materials reaching Earth's surface formed Earth's continental crust.7. According to paragraph 4, Earth's continental crustO has changed significantly in composition over timeO was as thick as Earth's mantle in its early stagesO is very thin relative to Earth's sizeO caused the temperatures of Earth's early core and mantle to gradually increaseParagraph 5:The lightest materials of all, including gases such as hydrogen and helium, bubbled through Earth's interior to the surface. So we can imagine the surface of the early Earth as a massive volcanic field. And we can judge pretty well what gases bubbled up to that surface by analyzing the mixture of gases emitted by volcanoes. These include hydrogen, helium, methane, water vapor, nitrogen, ammonia, and hydrogen sulfide. Other materials, including large amounts of water vapor, were brought in by cometary bombardments. Much of the hydrogenand helium escaped; but once Earth was fully formed, it was large enough for its gravitational field to hold most of the remaining gases, and these formed Earth's first stable atmosphere.8. What can be inferred from paragraph 5 about Earth's first stable atmosphere?O It existed before Earth was yet fully formed.O It contained very little hydrogen and helium.O It contained only materials that had bubbled up through Earth's surface.O It lacked water vapor.Paragraph 4:These lighter materials, such as the rocks we call granites, formed a layer of continental crust about 35 kilometers thick. ■Relative to Earth as a whole, this is as thin as an eggshell. ■Seafloor crust is even thinner, at about 7 kilometers; thus, even continental crust reaches only about 1/200th of the way to Earth's core. ■Much of the early continental crust has remained on Earth's surface to the present day.■9. Look at the four squares that indicate where the following sentence could be added to the passage.Even some of its oldest portions as old as 3.8 billion years can still be found in parts of Canada, Australia, South Africa, and Greenland.Where would the sentence best fit Click on a square to add the sentence to the passage.10. 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 answer choices do not belong in the summary because they express ideas that are not presented in the passage or are minor ideas in the passage. Thisquestion is worth 2 points. Drag your choices to the spaces where they belong. To review the passage, click on View Text.Answer ChoicesO Early Earth's lack of an atmosphere explains why it was bombarded with much more frequency and violence than other planetesimals.O Continued bombardments and internal pressures made the growing Earth hotter, causing its interior to melt and the heavier elements to sink and form Earth's core.O Lighter elements from Earth's interior rose and formed the mantle, a denser layer of silicates around the core, and the crust, a thinner layer of silicates at Earth's surface.O The formation of Earth's crust protected the inner layers of Earth from the high-energy particles in space, reducing the temperatures of the mantle and the core.O Once Earth had gone through the final stages of its formation, gases bubbled to the surface and were held by Earth's gravitational field to form the atmosphere.O Volcanoes today are the result of gases that were trapped in Earth's interior during the planet's early stages of formation.。
托福考试 复习托福阅读TPO16(试题+答案+译文)第3篇:Planets in Our Solar System托福阅读原文The Sun is the hub of a huge rotating system consisting of nine planets, their satellites, and numerous small bodies, including asteroids, comets, and meteoroids. An estimated 99.85 percent of the mass of our solar system is contained within the Sun, while the planets collectively make up most of the remaining 0.15 percent. The planets, in order of their distance from the Sun, are Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus, Neptune, and Pluto. Under the control of the Sun's gravitational force, each planet maintains an elliptical orbit and all of them travel in the same direction.The planets in our solar system fall into two groups: the terrestrial (Earth-like) planets (Mercury, Venus, Earth, and Mars) and the Jovian (Jupiter-like) planets (Jupiter, Saturn, Uranus, and Neptune). Pluto is not included in either category, because its great distance from Earth and its small size make this planet's true nature a mystery.The most obvious difference between the terrestrial and the Jovian planets is their size. The largest terrestrial planet, Earth has a diameter only one quarter as great as the diameter of the smallest Jovian planet, Neptune, and its mass is only one seventeenth as great. Hence, the Jovian planets are often called giants. Also, because of their relative locations,the four Jovian planets are known as the outer planets, while the terrestrial planets are known as the inner planets. There appears to be a correlation between the positions of these planets and their sizes. Other dimensions along which the two groups differ markedly are density and composition. The densities of the terrestrial planets average about 5 times the density of water, whereas the Jovian planets have densities that average only 1.5 times the density of water. One of the outer planets, Saturn, has a density of only 0.7 that of water, which means that Saturn would float in water. Variations in the composition of the planets are largely responsible for the density differences. The substances that make up both groups of planets are divided into three groups—gases, rocks, and ices—based on their melting points. The terrestrial planets are mostly rocks: dense rocky and metallic material, with minor amounts of gases. The Jovian planets, on the other hand, contain a large percentage of the gases hydrogen and helium, with varying amounts of ices: mostly water, ammonia, and methane ices.The Jovian planets have very thick atmospheres consisting of varying amounts of hydrogen, helium, methane, and ammonia. By comparison, the terrestrial planets have meager atmospheres at best. A planet's ability to retain an atmosphere depends on its temperature and mass. Simply stated, a gas molecule can "evaporate" from a planet if it reaches a speed known as the escape velocity. For Earth, this velocity is 11 kilometers persecond. Any material, including a rocket, must reach this speed before it can leave Earth and go into space. The Jovian planets, because of their greater masses and thus higher surface gravities, have higher escape velocities (21-60 kilometers per second) than the terrestrial planets. Consequently, it is more difficult for gases to "evaporate" from them. Also, because the molecular motion of a gas depends on temperature, at the low temperatures of the Jovian planets even the lightest gases are unlikely to acquire the speed needed to escape. On the other hand, a comparatively warm body with a small surface gravity, like Earth's moon, is unable to hold even the heaviest gas and thus lacks an atmosphere. The slightly larger terrestrial planets Earth, Venus, and Mars retain some heavy gases like carbon dioxide, but even their atmospheres make up only an infinitesimally small portion of their total mass.The orderly nature of our solar system leads most astronomers to conclude that the planets formed at essentially the same time and from the same material as the Sun. It is hypothesized that the primordial cloud of dust and gas from which all the planets are thought to have condensed had a composition somewhat similar to that of Jupiter. However, unlike Jupiter, the terrestrial planets today are nearly void of light gases and ices. The explanation may be that the terrestrial planets were once much larger and richer in these materials but eventually lost them because of these bodies' relative closeness to the Sun, which meant that theirtemperatures were relatively high.托福阅读试题1.According to the passage, each of the following statements comparing terrestrial planets with Jovian planets is true EXCEPT:A.Terrestrial planets are closer to the Sun than Jovian planets.B.Terrestrial planets have smaller diameters than Jovian planets.C.Terrestrial planets have smaller masses than Jovian planets.D.Terrestrial planets travel in a different direction than Jovian planets do.2.The word markedly in the passage (paragraph 4) is closest in meaning toA.EssentiallyB.TypicallyC.ConsistentlyD.Noticeably3.Paragraph 4 mentions which of the following as a reason why terrestrial planets are dense?A.They are made up of three groups of substances.B.They are composed mainly of rocky and metallic materials.C.They contain more ice than Jovian planets.D.They contain relatively small amounts of water.4.Paragraph 4 supports each of the following statements about Saturn EXCEPT:A.It is less dense than any of the terrestrial planets.B.It contains no rocky material.C.It contains ices.D.It contains a large percentage of gases.5.The word meager in the passage (paragraph 5) is closest in meaning toA.richB.thinC.uniqueplex6.According to paragraph 5, which of the following statements is true of both Jovian and terrestrial planets?A.The thicker the atmosphere, the smaller the planet’s massB.The more varied the gases in the atmosphere, the higher the temperatureC.The higher the surface gravity, the higher the escape velocityD.The less the atmosphere contributes to the total mass, the lower the temperature7.According to paragraph 5, what is a major reason that Jovian planets have much thicker atmospheres than terrestrial planets do?A.Jovian planets have lower surface gravitiesB.Jovian planets have lower temperaturesC.Jovian planets have lower escape velocitiesD.Jovian planets’ gas molecules have higher average speeds8.Paragraph 5 supports which of the following statements about the ability of planets to retain gases?A.More-massive planets are less able to retain gases than less-massive ones.B.Planets are more likely to retain heavy gases than light gases.C.Jovian planets are unlikely to retain the lightest gases.D.Only terrestrial planets have been able to retain carbon dioxide.9.In calling the cloud of gas and dust from which the Sun and all the planets are thought to have condensed "primordial",(in paragraph 6) the author means that the cloud wasA.immense in sizeposed of similar particlesC.present at the very beginning of our solar system's formationD.created from a great variety of different materials10.The word eventually in the passage (paragraph 6) is closest in meaning toA.over timeB.long agoC.simplyD.certainly11.According to paragraph 6, what is a possible explanation for the lack of light gases and ices on terrestrial planets?A.The location of terrestrial planets caused them to lose some of the materials they once contained.B.Terrestrial planets were formed much later than Jovian planets.C.The composition of terrestrial planets was different from that of Jupiter.D.Terrestrial planets were formed out of different material than the Sun was.12. Look at the four squares [■] that indicate where the following sentence could be added to the passage. Where would the sentence best fit? This explains their relatively low densities.Paragraph 4: Other dimensions along which the two groups differ markedly are density and composition. The densities of the terrestrial planets average about 5 times the density of water, whereas the Jovian planets have densities that average only 1.5 times the density of water. One of the outer planets, Saturn, has a density of only 0.7 that of water, which means that Saturn would float in water. Variations in the composition of the planets are largely responsible for the density differences. ■【A】The substances that make up both groups of planets are divided into three groups—gases, rocks, and ices—based on their melting points. ■【B】The terrestrial planets are mostly rocks: dense rockyand metallic material, with minor amounts of gases. ■【C】The Jovian planets, on the other hand, contain a large percentage of the gases hydrogen and helium, with varying amounts of ices: mostly water, ammonia, and methane ices. ■【D】13.Directions: From the seven answer choices below, select the two phrases that correctly characterize the terrestrial planets and the three phrases that correctly characterize the Jovian planets. Drag each phrase you select into the appropriate column of the table. Two of the phrases will NOT be used. This question is worth 3 points.A.Have relatively small sizesB.Are grouped in the same category as PlutoC.Contain relatively high proportions of icesD.Have relatively high temperaturesE.Have densities that are generally lower than the density of waterF.Have relatively high escape velocitiesG.Have a composition closer to that of the cloud from which they condensed terrestrial1 )terrestrial planetsA B C D E F G2 )Jovian planetsA B C D E F G托福阅读答案1.EXCEPT题,排除法,问整个文章,所以应该关注各段的开头。
2020届江苏黄桥中学高三英语期末试题及答案第一部分阅读(共两节,满分40分)第一节(共15小题;每小题2分,满分30分)阅读下列短文,从每题所给的A、B、C、D四个选项中选出最佳选项AYou’re becoming an adult; your friends are changing; school is more challenging; and your life has more ups and downs than it used to. These books are just for you.Say Goodbye to Stressby Dr Jeff BrownKindle Edition $11.79Paperback $16.95Many have trouble getting their stress (压力) under control and want help. This new book will encourage stressed-out readers with its stories from people like them about how they resolved or rethought the stress in their lives, learned to let go of anxiety and worry, and improved their lives by dealing with stress.Find Your Inner Strengthby Amy NewmarkKindle Edition $7.99Paperback $12.75This powerful collection of stories will inspire (激励) you and help you find the inner strength to do with the challenges in your own life. We are stronger than we think.... when we have to be. These brave. courageous people are the role models that show us all what is possible.Random Acts of Kindnessby Amy NewmarkKindle Edition $12.99Paperback $17.77Make miracles happen for yourself and others. It’s easy. Just think outside the box and look around. There are so many ways that you can help—and it turns out the biggest beneficiary (受益人) may be you! Scientific studies have shown that “doing good” is not only good for others but also for the person doing it, making that person happier and healthier.Be the Best You Can Beby Amy NewmarkKindle Edition $10. 99Paperback $15.67This collection shows kids positive role models to follow in its stories about making good choices, havingconfidence, and doing the right things. Parents and grandparents will enjoy discussing the stories with children, making it a family event.1.How will you feel after reading Say Goodbye to Stress?A.Anxious.B.Awkward.C.Relaxed.D.Confused.2.What is unique about Find Your Inner Strength?A.It is written by a well-known author.B.It is the cheapest of the four books.C.It has role models for kids to follow.D.It shows one how to do good deeds.3.Which book is suitable for one who has no confidence?A.Say Goodbye to StressB.Find Your Inner StrengthC.Random Acts of KindnessD.Be the Best You Can BeBNextdoor,an online social network for neighbors,says it has attracted $60 million from early backers of technology giants,Google,Amazon and Facebook.The new investment,1ed by venture firm Kleiner Perkins Caufield & Byers and investment firm Tiger Global Management,values Nextdoor at more than $500 million,said a personfamiliar with the matter.Nextdoor members make Facebook-style postings,giving or seeking recommendations for services such as babysitters and yard maintenance or local retailers and restaurants. They also post about community issues such as parking,crimeand safety,or items for sale or loan.The investment sum emphasizes the appeal of businesses that can tap into the growing use of mobile devices,as well as social networking Perhaps the best current example is Twitter,which is preparing for an initial public offering that values the company at up to about $11 billion.“We’re all spending more time with our screens,more engaged,but I think data shows we’re less connected,”said John Doerr of Kleiner Perkins,mentioning his own experience of knowing few of his neighbors. Nextdoor,with its ability to introduce neighbors to each other,helps people regain the sense of connection,he said.Early next year,Nextdoor plans to expand to Canada,followed by Great Britain,Australia,and South Africa,chief executive NiravTolia said. While Nextdoor has not yet have made any profit after two years of operations,Tolia said he is not worried.“If we look at the great companies at this stage,none of them started to monetize this early in their evolution. ”Tolia said. “It’s all about getting the product right. ”Eventually,Nextdoor plans to tap into local advertising,he said.Nextdoor is currently used in 22,527 neighborhoods across the United States,up from 5,694 a year ago. Including the latest funding round,it has raised just over $100 million.4. What attitude do the early backers of technology grant hold towards Nextdoor?A. They doubt its value.B. They think poorly of it.C. They are in favor of it.D. They are worried about it.5. What is mainly discussed about Nextdoor in Paragraph 3?A. Its members.B. Its service.C. Its value.D. Its location.6. What is the author’s purpose of mentioning Twitter in Paragraph 4?A. To support his viewpoint.B. To post an advertisement.C. To introduce a network.D. To makea public offer.7. How does Nirav Tolia feel about the future of Nextdoor?A. Curious.B. Upset.C. Cautious.D. Optimistic.CWhen I was a child, I attained high grades in my academic study. However, I was physically uncoordinated because I was running too slowly. But for future college application, sport was a must. So I took up fencing (击剑) because I thought it required more strategy than athletic ability.Then I joined the school’s fencing team. My movements were clumsy compared to the seniors. One afternoon after a whole lesson’s failure, tears of frustration welled up in my eyes. One of my teammates approached me, “Could you tell me where your blade (剑) hit me?” She asked. I pointed to her right shoulder. She nodded and patted my stomach, “That’s where I hit you.” She had begun to walk away when I blurted out, “Want to practice together? Again?”We practiced until we both felt more confident. But it wasn’t just the two of us. All these girls were entirelywilling to share their knowledge with everyone, helping each other to grow.That afternoon, I watched a senior fencer execute a flawless attack admiringly. Something inside me suddenly bloomed. I realized later that it was love for both fencing and the fencing team.During the city championship, I was selected to fence. My opponent was the best fencer on her school’s team. “Ready, fence.” The match began. Suddenly, my opponent’s blade hit me. The score was 1-0.At the moment I could hear my teammates shouting, “Keep distance!” And the team captain’s voice was clear and commanding, “Parry, then disengage!”Fencing, unlike academics, wasn’t something I could succeed in by myself—even during an individual match, my teammates were still giving me advice. Unathletic as I was, I was proud to be an athlete and a teammate.I saw my blade tip bury itself into my opponent’s shoulder and the judge signaling that it was my point. I could taste the sweat on my lips, which were breaking out into a smile.8. Why did the author start to learn fencing?A. Because she needed to train her coordination.B. Because she thought it would be easier for her.C. Because she could not succeed in any other sport.D. Because she wanted to enter the school fencing team.9. How did the girls improve their fencing skills?A. By observing flawless attacks.B. By practicing on their own.C. By offering guidance to each other.D. By competing with other teams.10. What distinguishes fencing from academics according to the author?A. Strong determination.B. Hard work.C. Athletic strategy.D. Team support.11. How did the author feel when she got her point?A. Unbeatable and respectful.B. Sweaty and ashamed.C. Energetic and secure.D. Proud and thankful.DAvi Loeb, a scientist, believes that we are not alone in the universe. The belief fits withLoeb's alien spaceship theory that at least one alien spaceship might be flying over the orbit of Jupiter, which won the international attention last year.Astronomers inHawaiifound the first known interstellar object in late 2017. It was a bit of light moving so fastpast the sun that it could only have come from another star. Almost every astronomer on the planet was trying to figure out how the object, called “Oumuamua” got to our far-away part of the Milky way galaxy. “One possibility is that ‘Oumuamua’ is debris from an advanced technological equipment,” Loeb said. “Technology comes from another solar system just showed up at our door. ”“‘Oumuamua’ is not an alien spaceship,” Paul Sutter, another scientist wrote. He suggested Loeb was seeking publicity. Most scientists think “Oumuamua” is some sort of rock. They think it could be an icy wandering comet.Loeb says that “Oumuamua's” behavior means it can't be a block of rock shaped like a long photo. He thinks it's more likely an object that's very long and thin, perhaps like a long pancake or a ship's sail. Loeb says that if someone shows him evidence thatcontradictshis beliefs, he will immediately give in.Loeb believes himself a truth-teller and risk-taker in an age of very safe, too-quiet scientists. “The worst thing that can happen to me is that I would be relieved of my management duties, and that would give me even more time to focus on science,” Loeb says. He said he wouldn't mind giving up all the titles he had and returning to the Israeli farming village where he grew up.12. What does Loeb say about “Oumuamua”?A. It is an icy comet.B. It looks like a long photo.C. It is actually some sort of rock.D. It may come from another alien civilization.13. What does the underlined word “contradicts” in paragraph 4 probably mean?A.Goes against.B. Relies on.C. Turns to.D. Searches for.14. What do you think of Loeb?A. He is foolish.B. He is unsatisfied with his titles.C. He is a firm believer in scientific truth.D. He is uncertain about his career future.15. What's the best title for the text?A. Have Aliens Paid a Visit in Spaceships?B. Do We Really Know about Space Theory?C. Scientists Are Working on High TechnologyD. Astronomers Are Encouraging Space Travel第二节(共5小题;每小题2分,满分10分)阅读下面短文,从短文后的选项中选出可以填入空白处的最佳选项。
venus in transit原文总结"Venus in Transit" is a scientific event that occurs when the planet Venus passes directly between the Earth and the Sun, resulting in a small, dark dot moving across the face of the Sun. This phenomenon is relatively rare, with pairs of Venus transits occurring only once every 243 years on average.The earliest known observation of Venus in transit was made in 1639 by Jeremiah Horrocks and his friend William Crabtree. Since then, scientists have used these events to study the motions and properties of Venus, as well as to make important measurements for determining the size of our solar system.During a Venus transit, astronomers can use special equipment, such as telescopes with solar filters, to safely observe the event. By measuring the time it takes for Venus to cross the disk of the Sun, scientists can calculate the distance between Earth and Venus, known as the astronomical unit (AU). This measurement is critical for estimating the sizes and distances of other planets and celestial objects.Venus transits also provide opportunities to search for extrasolar planets, or planets orbiting stars outside our solar system. When a planet passes in front of a distant star, it causes a slight dimming in the star's brightness. Observing a Venus transit can help researchers understand the techniques needed to detect these exoplanets and refine methods for studying their atmospheres. Overall, Venus in Transit is an important astronomical event that allows scientists to conduct research on our own solar system andbeyond. It provides valuable data for understanding the cosmos and contributes to our knowledge of the universe.。
高二英语天文理解练习题40题1<背景文章>The solar system is a fascinating place. It consists of the sun, eight planets, dwarf planets, moons, asteroids, comets, and other celestial bodies. The sun is at the center of the solar system and is a massive ball of hot gas. It provides light and heat to all the planets.The eight planets in our solar system are Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus, and Neptune. Each planet has its own unique characteristics. Mercury is the closest planet to the sun and is very hot. It has a rocky surface and no atmosphere to speak of. Venus is known as the Earth's sister planet because of its similar size and composition. However, it has a thick atmosphere of carbon dioxide, which makes it extremely hot.Earth is the only planet known to support life. It has a moderate climate, a large amount of water, and an atmosphere that is just right for living things. Mars is often called the Red Planet because of its reddish color. It has a thin atmosphere and evidence of past water on its surface.Jupiter is the largest planet in the solar system. It is a gas giant with a thick atmosphere of hydrogen and helium. Saturn is also a gas giant and is known for its beautiful rings. Uranus and Neptune are ice giants and are much farther from the sun.The planets in the solar system orbit the sun in elliptical paths. The closer a planet is to the sun, the faster it moves. The farther away a planet is, the slower it moves.1. Which planet is closest to the sun?A. VenusB. MercuryC. EarthD. Mars答案:B。
高二英语天文积累单选题40题1. Scientists have found evidence of water on Mars in the past few years. Which of the following statements about Mars is correct?A. Mars has a thick atmosphere like Earth.B. Mars is the closest planet to the Sun.C. Mars has polar ice caps.D. Mars has no volcanoes.答案:C。
解析:选项A,火星的大气层非常稀薄,不像地球那样浓厚,所以A错误。
选项B,离太阳最近的行星是水星,不是火星,B错误。
选项C,火星有极地冰盖,这是已经被探测到的,C正确。
选项D,火星上有火山,D错误。
这道题主要考查关于火星的基本天文知识以及对相关词汇的理解。
2. Venus is often called Earth's "sister planet" because of its similar size. However, there are significant differences. Which one is a major difference?A. Venus has no mountains.B. Venus rotates in the opposite direction compared to most planets.C. Venus has a moon.D. Venus has a very cold surface.答案:B。
解析:选项A,金星有山脉,A错误。
选项B,金星与大多数行星相比,自转方向相反,这是它和地球的一个重要区别,B正确。
选项C,金星没有卫星,C错误。
选项D,金星表面温度非常高,而不是很冷,D错误。
高二英语天文积累单选题40题1. The Earth is the third planet from the Sun. Which of the following statements about the Earth is correct?A. It has the shortest day among all the planets in the solar systemB. It is the largest planet in the solar systemC. It is the only planet known to support lifeD. It has no atmosphere答案:C。
解析:选项A,太阳系中木星的自转速度非常快,它的一天是最短的,而不是地球,所以A错误。
选项B,太阳系中最大的行星是木星,不是地球,所以B错误。
选项C,地球是目前已知唯一存在生命的行星,这是正确的。
选项D,地球有大气层,这对生命的存在有着重要意义,所以D错误。
2. Mars is often called the "Red Planet" because of its reddish appearance. What causes this color?A. High content of water on its surfaceB. Abundance of iron oxide on its surfaceC. A large amount of green plants on itD. The reflection of the Sun's red light答案:B。
解析:选项A,火星表面并没有大量的水,而且水不会使火星呈现红色,所以A错误。
选项B,火星表面富含氧化铁,这使得它呈现出红色,B正确。
选项C,火星上没有大量的绿色植物,所以C错误。
选项D,不是太阳红光的反射导致火星呈现红色,而是其表面物质的原因,所以D错误。
a r X i v :a s t r o -p h /0603376v 1 14 M a r 2006When Extrasolar Planets Transit Their Parent StarsDavid CharbonneauHarvard-Smithsonian Center for AstrophysicsTimothy M.BrownHigh Altitude ObservatoryAdam BurrowsUniversity of ArizonaGreg LaughlinUniversity of California,Santa CruzWhen extrasolar planets are observed to transit their parent stars,we are granted unprece-dented access to their physical properties.It is only for transiting planets that we are permitted direct estimates of the planetary masses and radii,which provide the fundamental constraints on models of their physical structure.In particular,precise determination of the radius may indicate the presence (or absence)of a core of solid material,which in turn would speak to the canonical formation model of gas accretion onto a core of ice and rock embedded in a protoplanetary disk.Furthermore,the radii of planets in close proximity to their stars are affected by tidal effects and the intense stellar radiation.As a result,some of these “hot Jupiters”are significantly larger than Jupiter in radius.Precision follow-up studies of such objects (notably with the space-based platforms of the Hubble and Spitzer Space Telescopes )have enabled direct observation of their transmission spectra and emitted radiation.These data provide the first observational constraints on atmospheric models of these extrasolar gas giants,and permit a direct comparison with the gas giants of the Solar system.Despite significant observational challenges,numerous transit surveys and quick-look radial velocity surveys are active,and promise to deliver an ever-increasing number of these precious objects.The detection of transits of short-period Neptune-sized objects,whose existence was recently uncovered by the radial-velocity surveys,is eagerly anticipated.Ultra-precise photometry enabled by upcoming space missions offers the prospect of the first detection of an extrasolar Earth-like planet in the habitable zone of its parent star,just in time for Protostars and Planets VI.1.OVERVIEWThe month of October 2005,in which the fifth Protostars and Planets meeting was held,marked two important events in the brief history of the observational study of planets or-biting nearby,Sun-like stars.First,it was the ten-year an-niversary of the discovery of 51Pegb (Mayor and Queloz ,1995),whose small orbital separation implied that similar hot Jupiters could be found in orbits nearly co-planar to our line of sight,resulting in mutual eclipses of the planet and star.Second,October 2005heralded the discovery of the ninth such transiting planet (Bouchy et al.,2005a).This se-lect group of extrasolar planets has enormous influence on our overall understanding of these objects:The 9transiting planets are the only ones for which we have accurate esti-mates of key physical parameters such as mass,radius,and,by inference,composition.Furthermore,precise monitor-ing of these systems during primary and secondary eclipse has permitted the direct study of their atmospheres.As a result,transiting planets are the only ones whose physicalstructure and atmospheres may be compared in detail to the planets of the Solar system,and indeed October 2005was notable for being the month in which the number of objects in the former category surpassed the latter.Our review of this rapidly-evolving field of study pro-ceeds as follows.In Section 2,we consider the physical structure of these objects,beginning with a summary of the observations (Section 2.1)before turning to their impact on our theoretical understanding (Section 2.2).In Section 3,we consider the atmospheres of these planets,by first sum-marizing the challenges to modeling such systems (Sec-tion 3.1),and subsequently reviewing the detections and upper limits,and the inferences they permit (Section 3.2).We end by considering the future prospects (Section 4)for learning about rocky planets beyond the Solar system through the detection and characterization of such objects in transiting configurations.2.PHYSICAL STRUCTURE2.1.Observations2.1.1.Introduction.When a planet transits,we can ac-curately measure the orbital inclination,i,allowing us to evaluate the planetary mass M pl directly from the minimum mass value M pl sin i determined from radial-velocity obser-vations and an estimate of the stellar mass,M⋆.The plane-tary radius,R pl,can be obtained by measuring the fraction of the parent star’s light that is occulted,provided a reason-able estimate of the stellar radius,R⋆,is available.With the mass and radius in hand,we can estimate such criti-cally interesting quantities as the average density and sur-face gravity.Hence,the information gleaned from the tran-siting planets allows us to attempt to unravel the structure and composition of the larger class of extrasolar planets, to understand formation and evolution processes(including orbital evolution),and to elucidate physical processes that may be important in planetary systems generically.Fig.1 shows the mass-radius relation for the9known transiting planets,with Jupiter and Saturn added for comparison.It is fortunate that the present small sample of objects spans a moderate range in mass and radius,and appears to contain both a preponderance of planets whose structure is fairly well described by theory,as well as a few oddities that chal-lenge our present knowledge.We begin by describing how the objects shown in Fig.1 were identified and characterized,and,along the way,we illuminate the limitations that these methods imply for our efforts to understand extrasolar planets as a class.By def-inition,transiting planets have their orbits oriented so that the Earth lies nearly in their orbital plane.This is an uncom-mon occurrence;assuming random orientation of planetary orbits,the probability that a planet with orbital eccentricity, e,and longitude of periastron,̟,produces transits visible from the Earth is given byP tr=0.0045 1AU R⊙ 1+e cos(π1−e2which is inversely proportion to a,the orbital semi-major axis.All known transiting planets have orbital eccentricities consistent with zero,for which the last factor in the above equation reduces to unity.The radii of Jovian planets are typically only about10% of the stellar radii.The transits known to date result in a 0.3−3%diminution of the stellarflux reaching the Earth. These transits last for1.5−3.5hours,and accurate ground-based characterizations of these events are challenging.The paucity and subtlety of the transits make it necessary to use great care to reduce the random errors and systematic bi-ases that plague the estimation of the planets’fundamental properties(Section2.1.4).2.1.2.Methods of Detection.The presently-known tran-siting planets have all been detected by one of the two fol-lowing means,both foreseen by Struve(1952):(1)Photo-metric detection of transit-like events,with subsequent con-firmation of planetary status via radial-velocity measure-ments,and(2)radial-velocity detection of a planet with subsequent measurement of photometric transits.Radial velocity detection has the advantage that the planetary na-ture of the target object is generally unambiguous.Its dis-advantage is that it requires substantial observing time on large telescopes to identify each planetary system,and only then can the relatively cheap process of searching for pho-tometric transits begin.Direct photometric transit searches simultaneously monitor large numbers of stars in a given field of view,but suffer from a very high rate of astrophysi-cal false positives(Section2.1.3).Successful photometric transit searches have so far adopted one of two basic strategies,using either moderate-sized or very small telescopes to search either fainter or brighter stars.Five transiting planets(OGLE-TR-10b,56b, 111b,113b,and132b)have been detected by the Optical Gravitational Lensing Experiment(OGLE)survey(Udal-ski et al.,2002a,2002b,2002c,2003,2004),which uses a 1.3m telescope.The parent stars of these planets are faint (typically V=16.5).The large-telescope follow-up obser-vations needed to verify their planetary status,to measure the stellar reflex velocities,and to estimate the planetary masses and radii have been conducted by several groups (Bouchy et al.,2004,2005b;Dreizler et al.,2002;Konacki et al.,2003a,2003b,2004,2005;Moutou et al.,2004;Pont et al.,2004;and Torres et al.,2004a,2004b,2005).The Trans-Atlantic Exoplanet Survey(TrES)employed a network of3automated small-aperture(10cm),wide-field(6◦×6◦)telescopes(Brown and Charbonneau,2000; Dunham et al.,2004;Alonso,2005)to detect the planet TrES-1(Alonso et al.,2004;Sozzetti et al.,2004).Its parent star(V=11.8)is significantly brighter that the OGLE sys-tems,but fainter than the transiting-planet systems detected by radial-velocity surveys(below).Because of this relative accessibility,TrES-1has also been the subject of intensive follow-up observations,as detailed later in this review.Numerous other photometric transit surveys are active at the current time.The BEST(Rauer et al.,2005),HAT (Bakos et al.,2004),KELT(Pepper et al.,2004),Super-W ASP(Christian et al.,2005),Vulcan(Borucki et al., 2001),and XO(McCullough et al.,2005)surveys,and the proposed PASS(Deeg et al.,2004)survey all adopt the small-aperture,wide-field approach,whereas the EX-PLORE(Mallen-Ornelas et al.,2003)project employs larger telescopes to examine fainter stars.The benefits of surveying stellar clusters(Janes,1996;Pepper and Gaudi, 2005)have motivated several surveys of such systems,in-cluding EXPLORE/OC(von Braun et al.,2005),PISCES (Mochejska et al.,2005,2006),and STEPSS(Burke et al., 2004;Marshall et al.,2005).An early,stunning null result was the HST survey of34,000stars in the globular cluster 47Tuc,which points to the interdependence of the forma-tion and migration of hot Jupiters on the local conditions, namely crowding,metallicity,and initial proximity to O and B stars(Gilliland et al.,2000).Finally,three transiting planets werefirst discovered by0.00.51.01.52.0Mass (M Jup )0.5 1.0 1.5 R a d i u s (R J u p )Fig.1.—Masses and radii for the 9transiting planets,as well as Jupiter and Saturn.The data are tabulated in Table 1,and are gatheredfrom Bakos et al.,in preparation ,Bouchy et al.(2004,2005b),Brown et al.,in preparation ,Charbonneau et al.(2006),Holman et al.(2005),Knutson et al.(2006),Laughlin et al.(2005a),Moutou et al.(2004),Pont et al.(2004),Sato et al.(2006),Sozzetti et al.(2004),Torres et al.(2004a),and Winn et al.(2005).radial-velocity surveys.These include HD 209458b,the first transiting planet discovered (Charbonneau et al.,2000;Henry et al.,2000;Mazeh et al.,2001),and the two most recently discovered transiting planets,HD 149026b (Sato et al.,2005)and HD 189733b (Bouchy et al.,2005a).The latter two objects were uncovered by quick-look radial-velocity surveys targeted at identifying short-period planets of metal-rich stars (respectively,the N2K Survey,Fischer et al.,2005;and the Elodie Metallicity-Biased Search,da Silva et al.,2006).Given the preference of radial-velocity surveys for bright stars,it is not surprising that all three systems are bright (7.6<V <8.2),making them natural targets for detailed follow-up observations.As we shall see below,HD 209458b has been extensively studied in this fashion.Similar attention has not yet been lavished on the other two,but only because of their very recent discovery.2.1.3.Biases and False Alarms.Photometric transit surveys increase their odds of success by simultaneously observing as many stars as possible.Hence,their target starfields are moderately to extremely crowded,and the sur-veys must therefore work near the boundary of technical feasibility.The constraints imposed by the search method influence which kinds of planets are detected.Photometric transit searches are strongly biased in fa-vor of planets in small orbits,since such objects have a greater probability of presenting an eclipsing configuration (Section 2.1.1).Moreover,most transit searches require a minimum of 2(and usually 3)distinct eclipses to be ob-served,both to confirm the reality of the signal,and to per-mit an evaluation of the orbital period.Since larger orbits imply longer orbital periods and fewer chances for tran-sits to occur,small orbits are preferred for transit surveys with only a limited baseline.This is frequently the regime in which single-site surveys operate.However,multi-site surveys that monitor a given field for several months (e.g.HAT,TrES)frequently achieve a visibility (the fraction of systems of a given period for which the desired number of eclipse events would be observed)nearing 100%for peri-ods up to 6days.As a result,such surveys do not suffer this particular bias,although admittedly only over a lim-ited range of periods.Similarly,a stroboscopic effect can afflict single-site surveys,favoring orbital periods near in-teger numbers of days and may account for the tendency of the longer-period transiting planet periods to clump near 3and 3.5days (Pont et al.,2004,Gaudi et al.,2005).This situation occurs if the campaign is significantly shorter in duration than that required to achieve complete visibility across the desired range or orbital periods.However,for observing campaigns for which more than adequate phase coverage has been obtained,the opposite is true,and pe-riods near integer and half-integer values are disfavored.The limiting example of this situation would be a single-site campaign consisting of thousands of hours of observations,which nonetheless would be insensitive to systems with in-teger periods,if their eclipses always occur when the field is below the horizon.Most field surveys operate in a regime limited by thesignal-to-noise of their time series(which are typically searched by an algorithm than looks for statistically-significant,transit-like events,e.g.Kov´a cs et al.,2002), and for which the number of stars increases with decreas-ingflux(a volume effect).An important detection bias for surveys operating under such conditions has been discussed by Pepper et al.(2003)and described in detail by Gaudi et al.(2005),Gaudi(2005),and Pont et al.(2005).These surveys can more readily detect planets with shorter peri-ods and larger radii orbiting fainter stars,and since such stars correspond to a large distance(hence volume)they are much more numerous.As a result,any such survey will reflect this bias,which cannot be corrected merely by improving the cadence,baseline,or precision of the time series(although improving the latter will reduce the thresh-old of the smallest planets that may be detected).Most ongoing transit surveys are plagued by a high rate of candidate systems displaying light curves that precisely mimic the desired signal,yet are not due to planetary tran-sits.We can divide such false positives into three broad categories:Some are true statistical false positives,result-ing from selecting an overly-permissive detection threshold whereby the light-curve search algorithmflags events that result purely from photometric noise outliers(Jenkins et al., 2002).The second source is instrumental,due to erroneous photometry,often resulting from leakage of signal between the photometric apertures of nearby stars in a crowdedfield. However,the dominant form,which we shall term astro-physical false positives,result from eclipses among mem-bers of double-or multiple-star systems.Grazing eclipses in binary systems can result in transit-like signals with depths and durations that resemble planetary ones(Brown, 2003),and this effect is especially pronounced for candidate transits having depths greater than1%.(For equal-sized components,roughly20%of eclipsing systems have eclipse depths that are less than2%of the total light.)In these cases the eclipse shapes are dissimilar(grazing eclipses produce V-shapes,while planetary transits haveflat bottoms),but in noisy data,this difference can be difficult to detect.A false alarm may also occur when a small star transits a large one (e.g.,an M-dwarf eclipsing a main-sequence F star).Since the lowest-mass stars have Jupiter radii,it is not surprising that such systems mimic the desired signal closely:They produceflat-bottomed transits with the correct depths and rger stars eclipsing even larger primaries can also mimic the desired signal,but a careful analysis of the transit shape can often reveal the true nature of the system (Seager and Mallen-Ornelas,2003).Other useful diagnos-tics emerge from careful analysis of the light curve outside of eclipses.These can reveal weak secondary eclipses,pe-riodic variations due to tidal distortion or gravity darken-ing of the brighter component,or significant color effects. Any of these variations provides evidence that the eclips-ing object has a stellar mass as opposed to a planetary mass (Drake,2003;Sirko and Paczy´n ski,2003;Tingley,2004).In the absence of these diagnostics,the stellar nature of most companions is easily revealed by low-precision(1km s−1)radial velocity measurements,since even the lowest-mass stellar companions cause reflex orbital motions of tens of km s−1(for examples,see Latham,2003;Charbonneau et al.,2004;Bouchy et al.,2005b;Pont et al.,2005).The most troublesome systems are hierarchical triple stars in which the brightest star produces the bulk of the system’s light,and the two fainter ones form an eclipsing binary.In such cases,the depths of the eclipses are di-luted by light from the brightest member,and often radial velocity observations detect only the bright component as well.Given neither radial velocity nor photometric evi-dence for a binary star,such cases can easily be mistaken for transiting planets.Correct identification then hinges on more subtle characteristics of the spectrum or light curve, such as line profile shapes that vary with the orbital period (Mandushev et al.,2005;Torres et al.,2004b,2005),or color dependence of the eclipse depth(O’Donovan et al., 2006).Because of the large preponderance of false alarms over true planets,it is only after all of the above tests have been passed that it makes sense to carry out the resource-intensive high-precision radial-velocity observations that establish beyond question that the transiting object has a planetary mass.2.1.4.Determining the Radii and Masses.After transit-ing planets are identified,an arsenal of observing tools is available(and necessary)for their characterization.An ac-curate estimate of M pl requires precise radial-velocity mea-surements(from which the orbital elements P,e,and̟are also determined),as well as an estimate of M⋆.The former are gathered with high-dispersion echelle spectro-graphs fed by large telescopes.For bright parent stars,pre-cision of a few m s−1(compared to reflex orbital speeds of 50−200m s−1)can be obtained with convenient exposure times,so that uncertainties in the velocity measurements do not dominate the estimate of M pl.In this regime,the great-est source of uncertainty is the value of M⋆itself.Given the difficulty of estimating the ages offield stars,compar-ison with grids of stellar models(e.g.Girardi et al.,2002) suggests that mass estimates are likely to be in error by as much as5%.This uncertainty could be removed by measur-ing the orbital speed of the planet directly.Several efforts have sought to recover the reflected-light spectrum of the planet in a series of high-resolution stellar spectra spanning key phases of the orbital period,but have achieved only upper limits(Charbonneau et al.,1999;Collier Cameron et al.,2002;Leigh et al.,2003a,2003b).(These results also serve to constrain the wavelength-dependent planetary albedo,a topic to which we shall return in Section3.2.2.) For faint parent stars,the radial-velocity estimates become more expensive and problematic,and contribute signifi-cantly to thefinal error budget for M pl.Interestingly, the most intractable uncertainty concerning masses of non-transiting planets,namely the value of sin i,is exquisitely well-determined byfits to the transit light curve.Analysis of moderate-precision light curves(obtained with ground-based telescopes)nonetheless yield a tightTime from Transit Center (days)R e l a t i v e F l u xFig.2.—HST photometric light curves of transits of TrES-1(top;Brown et al.,in preparation )and HD 209458(bottom;Brown et al.2001,offset by −0.007for clarity).The shorter orbital period and the smaller size of the TrES-1star result in a transit that is shorter in duration than that of HD 209458.Similarly,the smaller star creates a deeper transit for TrES-1,despite the fact that HD 209458b is the larger planet;the planetary sizes also affect the duration of ingress and egress.The TrES-1data reveal a “hump”centered at a time of −0.01d.This is likely the result of the planet occulting a starspot (or complex of starspots)on the stellar surface.constraint on the ratio R pl /R ⋆.However,fits to such data exhibit a fundamental degeneracy amongst the parameters R pl ,R ⋆,and i ,whereby the planet and stellar radii may be reduced in proportion so as to preserve the transit depth,and the orbital inclination may be correspondingly increased so as to conserve the chord length across the star.The uncer-tainty in R pl is typically dominated by such degeneracies.Determining the value of R pl requires fitting eclipse curves (facilitated by the analytic formulae of Mandel and Agol ,2002)subject to independent estimates of M ⋆,R ⋆,and the stellar limb-darkening coefficients.If sufficient photomet-ric precision can be achieved,the value of R ⋆may be de-rived from the light curve itself.This results in a reduced uncertainty on the value of R pl ,due to its weaker depen-dence on M ⋆,(∆R pl /R pl )≃0.3(∆M ⋆/M ⋆);see Char-bonneau (2003).For illustrative examples of the degenera-cies that result from such fits,see Winn et al.(2005),Hol-man et al.(2005),and Charbonneau et al.(2006).HST has yielded spectacular transit light curves for two bright systems,HD 209458(Brown et al.,2001)and TrES-1(Brown et al.,in preparation ),which are shown in Fig.2.The typical precision of these lightcurves is 10−4per one-minute integration,sufficient to extract new information from relatively subtle properties of the light curve,such as the duration of the ingress and egress phases,and the curvature of the light curve near the transit center.In prac-tice,such data have permitted a simultaneous fit that yields estimates of R pl ,R ⋆,i ,and the stellar limb-darkening co-efficients,thus reducing the number of assumed parametersto one:M ⋆.Cody and Sasselov (2002)point out that the combined constraint on (M ⋆,R ⋆)is nearly orthogonal to that resulting from light-curve fitting,serving to reduce the uncertainty in R pl .Further improvements can result from the simultaneously fitting of multi-color photometry under assumed values for the stellar-limb darkening,which serves to isolate the impact parameter (hence i )of the planet’s path across the star and break the shared degeneracy amongst R pl ,R ⋆,and i (Jha et al.,2000;Deeg et al.,2001).Re-cently,Knutson et al.(2006)have analyzed a spectrophoto-metric HST dataset spanning 290−1060nm,and the com-bined effect of the constraints described above has been to permit the most precise determination of an exoplanet ra-dius to date (HD 209458b;R pl =1.320±0.025R Jup ).2.1.5.Further Characterization Measurements.High-resolution stellar spectra obtained during transits can be used to determine the degree of alignment of the planet’s orbital angular momentum vector with the stellar spin axis.As the planet passes in front of the star,it produces a char-acteristic time-dependent shift of the photospheric line pro-files that stems from occultation of part of the rotating stel-lar surface.This phenomenon is known as the Rossiter-McLaughlin effect (Rossiter ,1924;McLaughlin ,1924),and has long been observed in the spectra of eclipsing bi-nary stars.Queloz et al.(2000)and Bundy and Marcy (2000)detected this effect during transits of HD 209458.A full analytic treatment of the phenomenon in the context of transiting extrasolar planets has been given by Ohta etal.(2005).Winn et al.(2005)analyzed the extensive radial-velocity dataset of HD209458,including19measurements taken during transit.They found that the measurements of the radial velocity of HD209458during eclipse exhibit an effective half-amplitude of∆v≃55m s−1,indicat-ing a line-of-sight rotation speed of the star of v sin i⋆= 4.70±0.16km s−1.They also detected a small asymmetry in the Rossiter-McLaughlin anomaly,which they modeled as arising from an inclination,λ,of the planetary orbit rel-ative to the apparent stellar equator ofλ=−4.4◦±1.4◦. Interestingly,this value is smaller than theλ=7◦tilt of the solar rotation axis relative to the net angular momen-tum vector defined by the orbits of the solar system planets (see Beck and Giles,2005).Wolf et al.(2006)carried out a similar analysis for HD149026,and foundλ=12◦±14◦. For these planets,the timescales for tidal coplanarization of the planetary orbits and stellar equators are expected to be of order1012yr(Winn et al.,2005;Greenberg,1974;Hut, 1980),indicating that the observed value ofλlikely reflects that at the end of the planet formation process.Pertubations in the timing of planetary transits may be used to infer the presence of satellites or additional plan-etary companions(Brown et al.,2001;Miralda-Escud´e, 2002).Agol et al.(2005)and Holman and Murray(2005) have shown how non-transiting terrestrial-mass planets could be detected through timing anomalies.Although HST observations have yielded the most precise timing measure-ments to date(with a typical precision of10s;see tabulation for HD209458in Wittenmyer et al.,2005),the constraints from ground-based observations can nonetheless be used to place interesting limits on additional planets in the system, as was recently done for TrES-1(Steffen and Agol,2005).Precise photometry can also yield surprises,as in the “hump”seen in Fig.2.This feature likely results from the planet crossing a large sunspot(or a complex of smaller ones),and thus is evidence for magnetic activity on the sur-face of the star.Such activity may prove to be an important noise source for timing measurements of the sort just de-scribed,but it is also an interesting object of study in its own right,allowing periodic monitoring of the stellar activ-ity along an isolated strip of stellar latitude(Silva,2003).2.2.Theory and Interpretation2.2.1.Overview and Uncertainties.Transiting planets give us the opportunity to test our understanding of the physical structure of giant planets.In particular,structural models of the known transiting planets must be able to ac-count for the wide range of radiationfluxes to which these planets are subjected,and they must recover the observed range of radii.In general,as the planetary mass decreases,a given external energy input has an increasingly larger influ-ence on the size and interior structure of the planet.For hot Jupiters,the absorbed stellarflux creates a radiative zone in the subsurface regions that controls the planetary contrac-tion,and ultimately dictates the radius.Models of transiting giant planets straddle the physical characteristics of brown dwarfs and low-mass stars,as well as the solar system gi-ants(for an overall review,see Burrows et al.,2001).The construction of structural models for giant planets is difficult because a number of key physical inputs are poorly constrained.This situation holds equally for extra-solar planets and for the exquisitely observed outer planets of the Solar system.A benefit of robust determinations of the parameters for a growing range of planets is that un-certain aspects of the theory can become increasingly con-strained.Indeed,transit observations have the potential to clarify some of the core questions regarding giant planets.The dominant uncertainty regarding the overall structure of gas giants is in the equation of state(see the review of Guillot,2005).The interiors of solar system and extrasolar giant planets consist of partially degenerate,partially ion-ized atomic-molecularfluids(Hubbard,1968).The pres-sure,P,in the interiors of most giant planets exceeds 10Mbar,and central temperatures range from T c≃104 for Uranus and Neptune to T c≃3×104for objects such as HD209458b.This material regime lies beyond the point where hydrogen ionizes and becomes metallic, although the details of the phase transition are still uncer-tain(Saumon et al.,2000;Saumon and Guillot,2004).The equation of state of giant planet interiors is partially acces-sible to laboratory experiments,including gas-gun(Holmes et al.,1995),laser-induced shock compression(Collins et al.,1998),pulsed-power shock compression(Knudson et al.,2004),and convergent shock wave(Boriskov et al., 2003)techniques.These experiments can achieve momen-tary pressures in excess of1Mbar,and they appear to be approaching the molecular to metallic hydrogen transition. Unfortunately,these experiments report diverging results. In particular,they yield a range of hydrogen compression factors relevant to planetary cores that differ by∼50%. Furthermore,the laboratory experiments are in only partial agreement withfirst-principles quantum mechanical cal-culations of the hydrogen equation of state(Militzer and Ceperley,2001;Desjarlais,2003;Bonev et al.,2004),and uncertainties associated with the equations of state of he-lium and heavier elements are even more severe(Guillot, 2005).At present,therefore,structural models must adopt the pragmatic option of choosing a thermodynamically con-sistent equation of state that reproduces either the high-or low-compression results(Saumon and Guillot,2004).Another uncertainty affecting the interior models is the existence and size of a radial region where helium separates from hydrogen and forms downward-raining droplets.The possibility that giant planet interiors are helium-stratified has non-trivial consequences for their structures,and ulti-mately,their sizes.In the case of Saturn,the zone of helium rain-out may extend all the way to the center,possibly re-sulting in a distinct helium shell lying on top of a heavier element core(Fortney and Hubbard,2003).Uncertainties in the equation of state,the bulk compo-sition,and the degree of inhomogeneity allow for a de-pressingly wide range of models for the solar system giants that are consistent with the observed radii,surface tempera-。