託福閱讀多選題多少分
託福閱讀部分，多選題內容的難度會更大，那麼相應的分數也會比較高。那麼具體的託福閱讀中，都有哪些題目是多選題，算分方法是怎樣的呢?爲了讓大家更好的來積累練習這部分內容，下面小編爲大家整理了詳細的內容，供大家參考!
託福閱讀多選題多少分
填表題，SUMMARY 3空2分，答對2題給1分
CHART 5空3分題 對4拿2分 對3拿1分
7空4分題，對6拿3分 對5拿2分 對4拿1分
2015年托福考生經驗交流羣
由此可見，託福閱讀多選題的分值還是很高的，那麼，在託福閱讀考試過程，我們怎麼做到儘可能不失分呢?首先我們就要做到以下幾點：
1、如果在託福閱讀文章中有主題句，結合主題句
與主題句無關的，砍了，不是主要觀點的，埋了，最後那些與文章無關或着根本就是錯的，拖出去槍斃5分鐘，剩下的基本上就是答案了。
2、一般人最容易犯的錯誤是將非主要觀點判斷爲主要觀點
我們可以採用的高分技巧就是看一看，他說的內容在整篇都談到了?還是隻有一段?如果全談到了，那麼就是主要，反之就不是。
託福閱讀背景知識：文明發展史
託福閱讀真題再現：
版本一： 講某個文明，說多個原因導致其發展。一是葡萄藤和橄欖樹的引入，和傳統農作物不衝突，無論土地還是收穫期。這使人們可以從事其他如鍊金屬青銅什麼的。然後這導致了不同group的爭鬥，爭奪資源和specialist。總體和某個TPO閱讀很像。
版本二：講希臘文明，全文大意一句總結：traditional analysis focused on external influences,but the professor thinks from the perspective of MUTIlieR EFFECT(考點)，which combined several interal impacts.
版本三：地中海地區某一時間一些國家的發展 A國發展之一種了Oliva什麼的一種長在島上不用在Farm上而且工人對這種作物的勞動時間也和其他作物不一樣，所以能大力發展，還有一種是Bronze的發展
解析： 本文講文明發展史。主要討論的是某文明發展的原因，主旨明確，結構清晰，每段首句爲topic sentence的可能性較高。大家在閱讀文章之前可以先跳到最後一題(文章總結題)的位置看看那句對於文章總結的句子。對於大家從整體上把握文章的結構非常有幫助。從文章結構與內容上，都非常接近TPO8的文章The Rise of Teotihucan。
託福閱讀相關背景：
Sumer
Sumer (from Akkadian ?umeru; Sumerian ki-en-?ir15, approximately "land of the civilized kings" or "native land"[note 1]) was an ancientcivilization and historical region in southern Mesopotamia, modern-day southern Iraq, during the Chalcolithic and Early Bronze Age. Although the earliest forms of writing in the region do not go back much further than c. 3500 BC, modern historians have suggested that Sumer was first permanently settled between c. 5500 and 4000 BC by a non-Semitic people who may or may not have spoken the Sumerian language (pointing to the names of cities, rivers, basic occupations, etc. as evidence).[1][2][3][4] These conjectured, prehistoric people are now called "proto-Euphrateans" or "Ubaidians",[5] and are theorized to have evolved from the Samarra culture of northern Mesopotamia (Assyria).[6][7][8][9] The Ubaidians were the first civilizing force in Sumer, draining the marshes for agriculture, developing trade, and establishing industries, including weaving, leatherwork, metalwork, masonry, and pottery.[5] However, some scholars such as Piotr Michalowski and Gerd Steiner, contest the idea of a Proto-Euphratean language or one substrate language. It has been suggested by them and others, that the Sumerian language was originally that of the hunter and fisher peoples, who lived in the marshland and the Eastern Arabia littoral region, and were part of theArabian bifacial culture.[10] Reliable historical records begin much later; there are none in Sumer of any kind that have been dated beforeEnmebaragesi (c. 26th century BC). Professor Juris Zarins believes the Sumerians were settled along the coast of Eastern Arabia, today's Persian Gulf region, before it flooded at the end of the Ice Age.[11] Sumerian literature speaks of their homeland being Dilmun.
Sumerologist Samuel Noah Kramer asserts "No people has contributed more to the culture of mankind than the Sumerians" and yet it is only comparatively recently that we have built up a knowledge of the existence of this ancient culture.[12] Sumerian civilization took form in theUruk period (4th millennium BC), continuing into the Jemdat Nasr and Early Dynastic periods. During the 3rd millennium BC, a close cultural symbiosis developed between the Sumerians (who spoke a language isolate) and the Semitic Akkadian speakers, which included widespreadbilingualism.[13] The influence of Sumerian on Akkadian (and vice versa) is evident in all areas, from lexical borrowing on a massive scale, tosyntactic, morphological, and phonological convergence.[13] This has prompted scholars to refer to Sumerian and Akkadian in the 3rd millennium BC as a sprachbund.[13] Sumer was conquered by the Semitic-speaking kings of the Akkadian Empire around 2270 BC (short chronology), but Sumerian continued as a sacred language. Native Sumerian rule re-emerged for about a century in the Third Dynasty of Ur (Sumerian Renaissance) of the 21st to 20th centuries BC, but the Akkadian language also remained in use. The Sumerian city of Eridu, on the coast of the Persian Gulf, was the world's first city, where three separate cultures fused - that of peasant Ubaidian farmers, living in mud-brick huts and practicing irrigation; that of mobile nomadic Semitic pastoralists living in black tents and following herds of sheep and goats; and that of fisher folk, living in reed huts in the marshlands, who may have been the ancestors of the Sumerians.[14]
The irrigated farming together with annual replenishment of soil fertility and the surplus of storable food in temple granaries created by this economy allowed the population of this region to rise to levels never before seen, unlike those found in earlier cultures of shifting cultivators. This much greater population density in turn created and required an extensive labour force and division of labour with many specialised arts and crafts. At the same time, historic overuse of the irrigated soils led to progressive salinisation, and a Malthusian crisis which led to depopulation of the Sumerian region over time, leading to its progressive eclipse by the Akkadians of middle Mesopotamia.
Sumer was also the site of early development of writing, progressing from a stage of proto-writing in the mid 4th millennium BC to writing proper in the 3rd millennium BC (see Jemdet Nasr period).
託福閱讀背景知識：動物遷徙
託福閱讀真題再現：
版本一：某些動物長大以後離開出生地生存，有些不會。主要講不可以的。舉了兩個例子。第一個是松鼠，雄鼠長大後飛走，雌鼠不會。第二個例子是獅子，雄獅子長大了以後會離開，原因是打不過原來的首領，被趕跑。雌性獅子則會留在羣落幫忙找吃的。
版本二：講動物離開出生點行爲，原因一：某鼠離開出生點，雄150米，雌50米，因爲能防止近親繁殖導致基因病，同時雌性在一起能養小鼠方便。原因二：獅子，羣內爭鬥呀，勞什子排擠呀什麼的。
版本三： 動物的disperse, 剛開始說爲什麼動物要離開熟悉的food rich的地方而去其他地方。其中講了一種動物男女的分佈是不一樣的，女的離原來的家50米，男的150米， 不同的原因是防止近親結婚導致孩子多病不易存活，另外女的離家近更有益處，家裏可以給她提供保護，然後男的要更遠的地方對抗敵人，有可能被競爭者replace而離開，然後有個lion的例子
託福閱讀詞彙：
squirrel n松鼠
disperse v分散
Inbreeding n近親交配
genopathy n遺傳病
解析：本文圍繞動物爲何離開出生地這個主題展開論證。做題時需注意記錄筆記，對於結構化閱讀及最後一題的解答有很大好處。動物行爲主題是託福閱讀常見考點，結構不難理解。需注意各例證和主題的支撐關係。由於條理清晰，最後一題儘量考慮從正面選出，排除爲輔。
託福閱讀相關背景：
Animal Inbreeding
Inbreeding is the production of offspring from the mating or breeding of individuals or organisms which are closely related genetically, in contrast to outcrossing, which refers to mating unrelated individuals.[1] By analogy, the term is used in human reproduction, but more commonly refers to the genetic disorders and other consequences that may arise from incestuous sexual relationships and consanguinity.
Inbreeding results in homozygosity, which can increase the chances of offspring being affected by recessive or deleterious traits.[2] This generally leads to a decreasedbiological fitness of a population,[3][4] (called inbreeding depression) which is its ability to survive and reproduce. An individual who inherits such deleterious traits is referred to as inbred. The avoidance of such deleterious recessive alleles caused by inbreeding is the main selective reason for outcrossing.[5][6]
Inbreeding is a technique used in selective breeding. In livestock breeding, breeders may use inbreeding when, for example, trying to establish a new and desirable traitin the stock, but will need to watch for undesirable characteristics in offspring, which can then be eliminated through further selective breeding or culling. Inbreeding is used to reveal deleterious recessive alleles, which can then be eliminated through assortative breeding or through culling. In plant breeding, inbred lines are used as stocks for the creation of hybrid lines to make use of the effects of heterosis. Inbreeding in plants also occurs naturally in the form of self-pollination.
Offspring of biologically related persons are subject to the possible impact of inbreeding, such as congenital birth defects. The chances of such disorders is increased the closer the relationship of the biological parents. (See coefficient of inbreeding.) This is because such pairings increase the proportion of homozygous zygotes in the offspring, in particular deleterious recessive alleles, that produce such disorders.[7] (See inbreeding depression.) Because most recessive alleles are rare in populations, it is unlikely that two unrelated marriage partners will both be carriers of the alleles. However, because close relatives share a large fraction of their alleles, the probability that any such deleterious allele is inherited from the common ancestor through both parents is increased dramatically. Contrary to common belief, inbreeding does not in itself alter allele frequencies, but rather increases the relative proportion of homozygotes to heterozygotes. However, because the increased proportion of deleterious homozygotes exposes the allele to natural selection, in the long run its frequency decreases more rapidly in inbred population. In the short term, incestuous reproduction is expected to produce increases in spontaneous abortions of zygotes, perinatal deaths, and postnatal offspring with birth defects.[8]
There may also be other deleterious effects besides those caused by recessive diseases. Thus, similar immune systems may be more vulnerable to infectious diseases (seeMajor histocompatibility complex and sexual selection).[9]
託福閱讀背景知識：如何判斷地質年齡
託福閱讀真題再現：
版本1:
文章先講太陽系裏的東西都有相同的起源。先是說所有的東西是在一起的，然後說地球由於地表的水、火山活動和一個什麼過程使得地球連最古老的石頭都沒有了。所以只能測定月球的隕石的成分了，結論是月球的表面和隕石的時間都是46億年。因爲月球表面沒有地球的這些活動，所以可以測定。
後面又說宇宙的星系都在不斷地拉開距離，通過星系的紅移可以確定距離還有速度，發現宇宙一直在膨脹。發現宇宙在137億年前是一個點。然後就有了宇宙大爆炸。
版本2： 講地球和宇宙年齡的測量。先說太陽系大部分物質是同一時間形成的，然後說地球年齡難是因爲誰腐蝕。接着引入一種物質，可以通過同位素測年齡。結果是和月球上的最古老的石頭近似。然後說宇宙在膨脹，大爆炸。通過紅移測年齡。
版本3： 天文類， 某種地球上的物質和月球上最古老的物質證明他。都始於自4.6million年前，於是證明太陽系的年齡是4.6 Million years. 另外還有種通過判斷各星球一種wavelength的大小推斷出他們在多少年前都是從個spot發展出來，於是判斷了big bang的時間。
託福閱讀相關詞彙：
origin 起源
meteorite 隕石
galaxy 星系
expansion 膨脹
red shift 紅移
wavelength 波長
解析：
天文主題文章的詞彙專業性較強，需要提前對相關專題的TPO文章的生詞熟悉，儘量減少生詞恐懼帶來的內耗。另外，出現天文理論的文章，結構通常都會比較清晰，但要着重識別對理論內容的態度傾向。
託福閱讀相關背景：
Bang
The Big Bang theory is the prevailing cosmological model for the early development of the universe. According to the theory, the Big Bang occurred approximately 13.82 billion years ago, which is thus considered the age of the universe. At this time, the universe was in an extremely hot and dense state and was expanding rapidly. After the initial expansion, the universe cooled sufficiently to allow the formation of subatomic particles, including protons, neutrons, and electrons. Though simple atomic nuclei formed within the first three minutes after the Big Bang, thousands of years passed before the first electrically neutral atoms formed. The majority of atoms that were produced by the Big Bang are hydrogen, along with helium and traces of lithium. Giant clouds of these primordial elements later coalesced through gravity to form stars and galaxies, and the heavier elements were synthesized either within stars or during supernovae.
lerating universe
The accelerating universe is the observation that the universe appears to be expanding at an increasing rate. In formal terms, this means that the cosmic scale factor has a positive second derivative,[1] so that the velocity at which a distant galaxy is receding from us should be continuously increasing with time.[2] In 1998, observations of type Ia supernovae also suggested that the expansion of the universe has been accelerating[3][4] since around redshift of z~0.5.[5] The 2006 Shaw Prize in Astronomy and the 2011 Nobel Prize in Physics were both awarded to Saul Perlmutter, Brian P. Schmidt, and Adam G. Riess, who in 1998 as leaders of the Supernova Cosmology Project (Perlmutter) and the High-Z Supernova Search Team (Schmidt and Riess) discovered the accelerating expansion of the Universe through observations of distant ("High-Z") supernovae.[6][7]
observations.[edit]
The simplest evidence for accelerating expansion comes from the brightness/redshift relation for distant Type-Ia supernovae; these are very bright exploding white dwarfs, whose intrinsic luminosity can be determined from the shape of the light-curve. Repeated imaging of selected areas of sky is used to discover the supernovae, and then followup observations give their peak brightness and redshift. The peak brightness is then converted into a quantity known as luminosity distance (see distance measures in cosmology for details).
For supernovae at redshift less than around 0.1, or light travel time less than 10 percent of the age of the universe, this gives a nearly linear redshift/distance relation due to Hubble's law. At larger distances, since the expansion rate of the universe has generally changed over time, the distance/redshift relation deviates from linearity, and this deviation depends on how the expansion rate has changed over time. The full calculation requires integration of the Friedmann equation, but the sign of the deviation can be given as follows: the redshift directly gives the cosmic scale factor at the time the supernova exploded, for example a supernova with a measured redshift implies the Universe was of its present size when the supernova exploded. In an accelerating universe, the universe was expanding more slowly in the past than today, which means it took a longer time to expand from 2/3 to 1.0 times its present size compared to a non-accelerating universe. This results in a larger light-travel time, larger distance and fainter supernovae, which corresponds to the actual observations: when compared to nearby supernovae, supernovae at substantial redshifts 0.2 - 1.0 are observed to be fainter (more distant) than is allowed in any homogeneous non-accelerating model.
Corroboration[edit]
After the initial discovery in 1998, these observations were corroborated by several independent sources: the cosmic microwave background radiation and large scale structure,[8] apparent size of baryon acoustic oscillations,[9] age of the universe,[10] as well as improved measurements of supernovae,[11][12] X-ray properties of galaxy clusters and Observational H(z) Data.[13]
Explanatory models[edit]
Models attempting to explain accelerating expansion include some form of dark energy, dark fluid or phantom energy. The most important property of dark energy is that it has negative pressure which is distributed relatively homogeneously in space. The simplest explanation for dark energy is that it is a cosmological constant or vacuum energy; this leads to the Lambda-CDM model, which has generally been known as the Standard Model of Cosmology from 2003 through the present, since it is the simplest model in good agreement with a variety of recent observations. Alternatively, some authors (e.g. Benoit-Lévy & Chardin[14], Hajdukovic[15], Villata[16]) have argued that the universe expansion acceleration could be due to a repulsive gravitational interaction of antimatter.
Theories for the consequences to the universe[edit]
As the Universe expands, the density of radiation and ordinary and dark matter declines more quickly than the density of dark energy (see equation of state) and, eventually, dark energy dominates. Specifically, when the scale of the universe doubles, the density of matter is reduced by a factor of 8, but the density of dark energy is nearly unchanged (it is exactly constant if the dark energy is a cosmological constant).
Current observations indicate that the dark energy density is already greater than the mass-energy density of radiation and matter (including dark matter). In models where dark energy is a cosmological constant, the universe will expand exponentially with time from now on, coming closer and closer to a de Sitter spacetime. In this scenario the time it takes for the linear size scale of the universe to expand to double its size is approximately 11.4 billion years. Eventually all galaxies beyond our own local supercluster will redshift so far that it will become hard to detect them, and the distant universe will turn dark.
In other models, the density of dark energy changes with time. In quintessence models it decreases, but more slowly than the energy density in ordinary matter and radiation. In phantom energy models it increases with time, leading to a big rip.
