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OG12 117

After evidence was obtained in the 1920s that
the universe is expanding, it became reasonable
to ask: Will the universe continue to expand
indefinitely, or is there enough mass in it for the
mutual attraction of its constituents to bring this
expansion to a halt? It can be calculated that
the critical density of matter needed to brake the
expansion and “close” the universe is equivalent
to three hydrogen atoms per cubic meter. But the
density of the observable universe—luminous matter
in the form of galaxies—comes to only a fraction
of this. If the expansion of the universe is to stop,
there must be enough invisible matter in the
universe to exceed the luminous matter in density
by a factor of roughly 70.
Our contribution to the search for this “missing
matter” has been to study the rotational velocity
of galaxies at various distances from their center
of rotation. It has been known for some time that
outside the bright nucleus of a typical spiral galaxy
luminosity falls off rapidly with distance from the
center. If luminosity were a true indicator of mass,
most of the mass would be concentrated toward
the center. Outside the nucleus the rotational
velocity would decrease geometrically with distance
from the center, in conformity with Kepler’s law.
Instead we have found that the rotational velocity
in spiral galaxies either remains constant with
increasing distance from the center or increases
slightly. This unexpected result indicates that the
falloff in luminous mass with distance from the
center is balanced by an increase in nonluminous
mass.
Our findings suggest that as much as 90
percent of the mass of the universe is not radiating
at any wavelength with enough intensity to be
detected on the Earth. Such dark matter could be
in the form of extremely dim stars of low mass,
of large planets like Jupiter, or of black holes,
either small or massive. While it has not yet been
determined whether this mass is sufficient to
close the universe, some physicists consider it
significant that estimates are converging on the
critical value.

117. The authors’ suggestion that “as much as 90 percent
of the mass of the universe is not radiating at any
wavelength with enough intensity to be detected on
the Earth” (lines 34–37) would be most weakened if
which of the following were discovered to be true?
(A) Spiral galaxies are less common than types of
galaxies that contain little nonluminous matter.
(B) Luminous and nonluminous matter are
composed of the same basic elements.
(C) The bright nucleus of a typical spiral galaxy also
contains some nonluminous matter.
(D) The density of the observable universe is
greater than most previous estimates have
suggested.
(E) Some galaxies do not rotate or rotate too slowly
for their rotational velocity to be measured
此题看不懂啊,哪位NN给解释下??
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你哪里看不明白~
题目说的是百分之九十宇宙中的物质是以任何波长具有足够的强度,能在地球上被发现的~
上一段说的是有螺旋的星系推出的结论,螺旋星系具有代表性质,我认为选着a
特殊削弱,只有说明螺旋星系不具有普遍性就好了呀~

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我还是不太明白。。上一段哪说螺旋星系有代表性质了呀?一直在说什么中心的距离增加减少什么的,看得我都晕了。。还说 不发光体平衡了 发光体和中心的距离的falloff。。。什么跟什么啊

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这里的our finding很明显指的是针对spiral galaxy的研究成果,因为之前段落"we"研究的只是spiral galaxy,而他们试图把这个星系的规律应用到整个宇宙。所以前提是spiral galaxy的组成结构具备代表性才行。A可以很好的削弱这个前提。

“一直在说什么中心的距离增加减少什么的”这描述的是spiral galaxy的具体特性。做这道题rainbow你没看懂细节也没关系的,关键是看到那个转承关系。

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天啊 这篇我觉得超级难啊,不看懂细节只看转承关系 这种很纠结的细节题可以做对吗?

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原來spiral galaxies是galaxies的一種阿,看懂了,這篇跟那篇有關于水的法律文章,是我覺得最難的文章.邏輯不明顯,不好找,考試上碰到這2篇,也只能放弃,考猜了

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原来跟这句话本身都没什么关系的,我一直在想怎么忽然扯到波长上来了。。

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那(E)呢? Some galaxies do not rotate or rotate too slowly for their rotational velocity to be measured
这项为什么不能削弱啊?假如那个旋转速度都测不到了,那怎么进行分析呢?OG解释说文章已经默认了这个旋转速度是可以预测的,可是我怎么知道哪些是默认的哪些是不默认的呢?~?~

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e这个我明白的,从意思上看,只要spiral galaxy具有代表性,足够多,就可以以对其的发现推广到整个宇宙,所以其中有一些特殊的galaxy,比如速度根本测不出也不会影响最终的结论。

我的问题是d,答案的解释我不明白啊。文中中旋转速度是由质量mass决定的,因为速度基本没变,所以推测暗物质要占总质量的90%才行,所以d中说亮物质的密度其实比测的的更高,其实是说暗物质的密度可以稍微低点,但是密度和质量其实并不是一回事,所以应该是“无关”才对,答案却说虽然亮物质的密度高了,也不会高过暗物质,实在是不明白这个解释说明了什么问题。。。

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ans E说如果不可测,那么这个finding根本就不可能存在.
题目要求是weaken,从逻辑上来讲这个finding首先要存在才能被weaken,如果它都不存在,根本就谈不上什么weaken的了.
至于ans D,这个答案是我最先排除的,我个人理解的是这个finding是围绕rotational velocity展开的,跟这个density没什么关系,也就是irrelevant了.

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