托福閱讀真題Official 50 Passage 3（一）

托福閱讀真題Official 50 Passage 3（一）

Star Death

Until the early-to mid-twentieth century,scientists believed that stars generate energy by shrinking.As stars contracted,it was thought,they would get hotter and hotter,giving off light in the process.This could not be the primary way that stars shine,however.If it were,they would scarcely last a million years,rather than the billions of years in age that we know they are.We now know that stars are fueled by nuclear fusion.Each time fusion takes place,energy is released as a by-product.This energy,expelled into space,is what we see as starlight.The fusion process begins when two hydrogen nuclei smash together to form a particle called the deuteron(a combination of a positive proton and a neutral neutron).Deuterons readily combine with additional protons to form helium.Helium,in turn,can fuse together to form heavier elements,such as carbon.In a typical star,merger after merger takes place until significant quantities of heavy elements are built up.

We must distinguish,at this point,between two different stellar types:Population I and Population II,the latter being much older than the former.These groups can also be distinguished by their locations.Our galaxy,the Milky Way,is shaped like a flat disk surrounding a central bulge.Whereas Population I stars are found mainly in the galactic disk,Population II stars mostly reside in the central bulge of the galaxy and in the halo surrounding this bulge.

Population II stars date to the early stages of the universe.Formed when the cosmos was filled with hydrogen and helium gases,they initially contained virtually no heavy elements.They shine until their fusible material is exhausted.When Population II stars die,their material is spread out into space.Some of this dust is eventually incorporated into newly formed Population I stars.Though Population I stars consist mostly of hydrogen and helium gas,they also contain heavy elements(heavier than helium),which comprise about 1 or 2 percent of their mass.These heavier materials are fused from the lighter elements that the stars have collected.Thus,Population I stars contain material that once belonged to stars from previous generations.The Sun is a good example of a Population I star.

What will happen when the Sun dies.In several billion years,our mother star will burn much brighter.It will expend more and more of its nuclear fuel,until little is left of its original hydrogen.Then,at some point in the far future,all nuclear reactions in the Sun’s center will cease.

Once the Sun passes into its“postnuclear”phase,it will separate effectively into two different regions:an inner zone and an outer zone.While no more hydrogen fuel will remain in the inner zone,there will be a small amount left in the outer zone.Rapidly,changes will begin to take place that will serve to tear the Sun apart.The inner zone,its nuclear fires no longer burning,will begin to collapse under the influence of its own weight and will contract into a tiny hot core,dense and dim.An opposite fate will await the outer region,a loosely held-together ball of gas.A shock wave caused by the inner zone’s contraction will send ripples through the dying star,pushing the stellar exterior’s material farther and farther outward.The outer envelope will then grow rapidly,increasing,in a short interval,hundreds of times in size.As it expands,it will cool down by thousands of degrees.Eventually,the Sun will become a red giant star,cool and bright.It will be so large that it will occupy the whole space that used to be the Earth’s orbit and so brilliant that it would be able to be seen with the naked eye thousands of light-years away.It will exist that way for millions of years,gradually releasing the material of its outer envelope into space.Finally,nothing will be left of the gaseous exterior of the Sun;all that will remain will be the hot,white core.The Sun will have become a white dwarf star.The core will shrink,giving off the last of its energy,and the Sun will finally die.

Question 1 of 14

The word“readily”in the passage is closest in meaning to

A.eventually

B.easily

C.constantly

D.loosely

正確答案：B

題目詳解

題型分類：詞匯題

選項(xiàng)分析：

原句為：聚變開始于兩個(gè)氫原子核碰撞在一起形成叫做氘核的微粒。氘核readily與其他的質(zhì)子結(jié)合形成氦?？梢酝茰y(cè)readily意為容易的，即B選項(xiàng)。

A選項(xiàng)eventually：最后地；錯(cuò)誤。氘核與其他質(zhì)子結(jié)合不是最后一步，后面還有氦聚變。

C選項(xiàng)constantly：不斷地。

D選項(xiàng)loosely：寬松地；放蕩地；輕率地。

Question 2 of 14

According to paragraph 1,the energy that comes from stars and that is seen as light is the result of

A.protons combining with helium atoms

B.atoms of heavier elements smashing together

C.various particles fusing with one another

D.hydrogen atoms breaking apart

Paragraph 1 is marked with an arrow

正確答案：C

題目詳解

題型分類：事實(shí)信息題

原文定位：根據(jù)light定位到第一段第七句。

選項(xiàng)分析：

根據(jù)定位句中有this energy，this表指代關(guān)系，應(yīng)該往前看第六句：每次聚變發(fā)生，能量就作為副產(chǎn)物被釋放；而這種能量我們看作星光。C選項(xiàng)various particles fusing對(duì)應(yīng)第六句fusion。

A選項(xiàng)：原文沒有說氦原子結(jié)合質(zhì)子，是氘核deuteron結(jié)合質(zhì)子。

B選項(xiàng)：原文只說了氫原子核碰撞，沒有說atoms of heavier elements碰撞。

D選項(xiàng)：原文說的是氫原子碰撞，而不是分裂。

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