- 最后登录
- 2015-7-22
- 在线时间
- 2534 小时
- 寄托币
- 26938
- 声望
- 1790
- 注册时间
- 2008-7-26
- 阅读权限
- 175
- 帖子
- 1414
- 精华
- 4
- 积分
- 14001
- UID
- 2522388
   
- 声望
- 1790
- 寄托币
- 26938
- 注册时间
- 2008-7-26
- 精华
- 4
- 帖子
- 1414
|
SECTION BUntil recently astronomers have been puzzled by the fate of red giant (red giant: n. 〈天〉红巨星a star that has low surface temperature and a diameter that is large relative to the sun) and supergiant stars. When the core of a giant star whose mass surpasses 1.4 times the present mass of our Sun (M⊙) exhausts its nuclear fuel, it is unable to support its own weight and collapses into a tiny neutron star (a hypothetical dense celestial object that consists primarily of closely packed neutrons and that results from the collapse of a much larger stellar body). The gravitational energy released during this implosion of the core blows off (blow off: v.吹掉, 放出) the remainder of the star in a gigantic explosion, or a supernova. Since around 50 percent of all stars are believed to begin their lives with masses greater than 1.4M⊙, we might expect that one out of every two stars would die as a supernova. But in fact, only one star in thirty dies such a violent death. The rest expire much more peacefully as planetary nebulas. Apparently most massive stars manage to lose sufficient material that their masses drop below the critical value of 1.4 M⊙ before they exhaust their nuclear fuel.
Evidence supporting this view comes from observations of IRC+10216, a pulsating giant star (a star of great luminosity and of large mass) located 700 light-years away from Earth. A huge rate of mass loss (1 M⊙ every 10,000 years) has been deduced from infrared observations of ammonia (NH3) molecules located in the circumstellar cloud around IRC+10216. Recent microwave observations of carbon monoxide (CO) molecules indicate a similar rate of mass loss and demonstrate that the escaping material extends outward from the star for a distance of at least one light-year. Because we know the size of the cloud around IRC+10216 and can use our observations of either NH3 or CO to measure the outflow velocity, we can calculate an age for the circumstellar cloud. IRC+10216 has apparently expelled, in the form of molecules and dust grains, a mass equal to that of our entire Sun within the past ten thousand years. This implies that some stars can shed huge amounts of matter very quickly and thus may never expire as supernovas. Theoretical models as well as statistics on supernovas and planetary nebulas suggest that stars that begin their lives with masses around 6 M⊙ shed sufficient material to drop below the critical value of 1.4 M⊙. IRC+10216, for example, should do this in a mere 50,000 years from its birth, only an instant in the life of a star.
But what place does IRC+10216 have in stellar evolution? Astronomers suggest that stars like IRC+10216 are actually “protoplanetary nebulas”—old giant stars whose dense cores have almost but not quite rid themselves of the fluffy envelopes of gas around them. Once the star has lost the entire envelope, its exposed core becomes the central star of the planetary nebula (a usually compact luminous ring-shaped nebula that is composed of matter which has been ejected from a hot star at its center) and heats and ionizes the last vestiges of the envelope as it flows away into space. This configuration is a full-fledged planetary nebula, long familiar to optical astronomers.
脉络分析:第一段 puzzle的问题所在。
第二三段:分析特例IRC。
21.
The primary purpose of the passage is to
(A) offer a method of calculating the age of circumstellar clouds
(B) describe the conditions that result in a star’s expiring as a supernova
(C) discuss new evidence concerning the composition of planetary nebulas
(D) explain why fewer stars than predicted expire as supernovas(D)
(E) survey conflicting theories concerning the composition of circumstellar clouds
Until recently astronomers have been puzzled by the fate of red giant (red giant: n. 〈天〉红巨星a star that has low surface temperature and a diameter that is large relative to the sun) and supergiant stars. When the core of a giant star whose mass surpasses 1.4 times the present mass of our Sun (M⊙) exhausts its nuclear fuel, it is unable to support its own weight and collapses into a tiny neutron star (a hypothetical dense celestial object that consists primarily of closely packed neutrons and that results from the collapse of a much larger stellar body).
22.
The passage implies that at the beginning of the life of IRC+10216, its mass was approximately
(A) 7.0 M⊙
(B) 6.0 M⊙
(C) 5.0 M⊙
(D) 1.4 M⊙(B)
(E) 1.0 M⊙
that stars that begin their lives with masses around 6 M⊙ shed sufficient material to drop below the critical value of 1.4 M⊙.
IRC+10216, for example, should do this in a mere 50,000 years from its birth, only an instant in the life of a star.
23.
The view to which line 18 refers serves to
(A) reconcile seemingly contradictory facts 由but in fact 直接推出。与reconcile完美对应
(B) undermine a previously held theory
(C) take into account data previously held to be insignificant
(D) resolve a controversy(A)
(E) question new methods of gathering data
But in fact, only one star in thirty dies such a violent death. The rest expire much more peacefully as planetary nebulas.
24.
It can be inferred from the passage that the author assumes which of the following in the discussion of the rate at which IRC+10216 loses mass?
(A) The circumstellar cloud surrounding IRC+10216 consists only of CO and NH3 molecules.
(B) The circumstellar cloud surrounding IRC+10216 consists of material expelled from that star.
(C) The age of a star is equal to that of its circumstellar cloud.
(D) The rate at which IRC+10216 loses mass varies significantly from year to year.(B)
(E) Stars with a mass greater than 6 M⊙ lose mass at a rate faster than stars with a mass less than 6 M⊙ do.
A huge rate of mass loss (1 M⊙ every 10,000 years) has been deduced from infrared observations of ammonia (NH3) molecules located in the circumstellar cloud around IRC+10216. Recent microwave observations of carbon monoxide (CO) molecules indicate a similar rate of mass loss and demonstrate that the escaping material extends outward from the star for a distance of at least one light-year.
25.
According to information provided by the passage, which of the following stars would astronomers most likely describe as a planetary nebula?
(A) A star that began its life with a mass of 5.5 M⊙, has exhausted its nuclear fuel, and has a core that is visible to astronomers
(B) A star that began its life with a mass of 6 M⊙, lost mass at a rate of 1 M⊙ per 10,000 years, and exhausted its nuclear fuel in 40,000 years
(C) A star that has exhausted its nuclear fuel, has a mass of 1.2 M⊙, and is surrounded by a circumstellar cloud that obscures its core from view
(D) A star that began its life with a mass greater than 6 M⊙, has just recently exhausted its nuclear fuel, and is in the process of releasing massive amounts of gravitational energy(A)
(E) A star that began its life with a mass of 5.5 M⊙, has yet to exhaust its nuclear fuel, and exhibits a rate of mass loss similar to that of IRC+10216
Once the star has lost the entire envelope, its exposed core becomes the central star of the planetary nebula (a usually compact luminous ring-shaped nebula that is composed of matter which has been ejected from a hot star at its center) and heats and ionizes the last vestiges of the envelope as it flows away into space. This configuration is a full-fledged planetary nebula, long familiar to optical astronomers.
Lost Entire envelope即exhausted its nuclear fuel.
Long familiar to optical astronomers 即 visible to astronomers 至于5,5.、纯是比6小的然后就Not enough large。
26.
Which of the following statements would be most likely to follow the last sentence of the passage?
(A) Supernovas are not necessarily the most spectacular events that astronomers have occasion to observe.
(B) Apparently, stars that have a mass of greater than 6 M⊙ are somewhat rare.
(C) Recent studies of CO and NH3 in the circumstellar clouds of stars similar to IRC+10216 have led astronomers to believe that the formation of planetary nebulas precedes the development of supernovas.
(D) It appears, then, that IRC+10216 actually represents an intermediate step in the evolution of a giant star into a planetary nebula.(D)
(E) Astronomers have yet to develop a consistently accurate method for measuring the rate at which a star exhausts its nuclear fuel.
LAST SENTENCE: This configuration is a full-fledged planetary nebula, long familiar to optical astronomers.
这道题只能一个个比较关系了。 前面在说 IRC为giant star难以直接被发现。然后末尾在说一个Once the star has lost the entire envelope, 即只有giant star 变小后才可以实现 long familiar to 。那么接下来一句不是说 因此,IRC变成了planetary nebula么。
27.
Which of the following titles best summarizes the content of the passage?
(A) New Methods of Calculating the Age of Circumstellar Clouds
(B) New Evidence Concerning the Composition of Planetary Nebulas
(C) Protoplanetary Nebula: A Rarely Observed Phenomenon
(D) Planetary Nebulas: An Enigma to Astronomers(E)
(E) The Diminution of a Star’s Mass: A Crucial Factor in Stellar Evolution
见全文脉络分析。
因为时间有限,所以做得比较仓促。请各位多多包涵。如果有什么问题,请在附加在这后面。我晚上回来解答。谢谢。 |
-
总评分: 寄托币 + 5
查看全部投币
|