[悦读] 柒月石日起悦读寂静整理（共45只。更新至8\3-20:15）

企鹅妮

辛苦楼主了！

silviapan

谢谢楼主，祈祷8月14不换库！

小晴子来啦

楼主大大大好人！！！

chenlencu

楼主真好

huangkang3039

Sally,
我看阅读JJ16题的时候，还是觉得特别晕，不怎么看的懂，在网上搜了一下，有一篇类似的文章，讲差不多一回事的东西，可以更新在JJ里面给大家个参考哈！这种宇宙太空题最头痛了。。。

As a heavy, stable particle, the lightest neutralino is an excellent candidate to comprise the universe's cold dark matter. In many models the lightest neutralino can be produced thermally in the hot early universe and leave approximately the right relic abundance to account for the observed dark matter. A lightest neutralino of roughly 10–10000 Ge V is the leading weakly interacting massive particle (WIMP) dark matter candidate.
　　Neutralino dark matter could be observed experimentally in nature either indirectly or directly. In the former case, gamma ray and neutrino telescopes look for evidence of neutralino annihilation in regions of high dark matter density such as the galactic or solar center. In the latter case, special purpose experiments such as the Cryogenic Dark Matter Search (CDMS) seek to detect the rare impacts of WIMPs in terrestrial detectors. These experiments have begun to probe interesting super symmetric parameter space, excluding some models for neutralino dark matter, and upgraded experiments with greater sensitivity are under development.

huangkang3039

从WIKI 上找的课外阅读补充材料，有兴趣的可以看一看，大致的生词什么的都在里面。 GMAT考这种东西真是变态啊，抱着有道一路查字典，才迷迷糊糊的明白到底咋回事。希望自己能够熟悉这些莫名其妙的单词，考试时候碰到不会太紧张短路。 ：）

History of the search for dark matter composition

Although dark matter had historically been inferred by many astronomical observations, its composition long remained speculative. Early theories of dark matter concentrated on hidden heavy normal objects, such as black holes, neutron stars, faint old white dwarfs, brown dwarfs, as the possible candidates for dark matter, collectively known as MACHOs. Astronomical surveys failed to find enough of these hidden MACHOsSome hard-to-detect baryonic matter, such as MACHOs and some forms of gas, were additionally speculated to make a contribution to the overall dark matter content, but evidence indicated such would constitute only a small portion. Furthermore, data from a number of lines of other evidence, including galaxy rotation curves, gravitational lensing, structure formation, and the fraction of baryons in clusters and the cluster abundance combined with independent evidence for the baryon density, indicated that 85–90% of the mass in the universe does not interact with the electromagnetic force. This "nonbaryonic dark matter" is evident through its gravitational effect. Consequently, the most commonly held view was that dark matter is primarily non-baryonic, made of one or more elementary particles other than the usual electrons, protons, neutrons, and known neutrinos. The most commonly proposed particles then became WIMPs (Weakly Interacting Massive Particles, including neutralinos), or axions, or sterile neutrinos, though many other possible candidates have been proposed.
The dark matter component has much more mass than the "visible" component of the universe.[63] Only about 4.6% of the mass-energy of the Universe is ordinary matter. About 23% is thought to be composed of dark matter. The remaining 72% is thought to consist of dark energy, an even stranger component, distributed almost uniformly in space and with energy density non-evolving or slowly evolving with time [64] Determining the nature of this dark matter is one of the most important problems in modern cosmology and particle physics. It has been noted that the names "dark matter" and "dark energy" serve mainly as expressions of human ignorance, much like the marking of early maps with "terra incognita".
Historically, three categories of dark matter candidates had been postulated. The categories cold, warm, and hot refer to how far the particles could move due to random motions in the early universe, before they slowed down due to the expansion of the Universe - this is called the "free streaming length". Primordial density fluctuations smaller than this free-streaming length get washed out as particles move from overdense to underdense regions, while fluctuations larger than the free-streaming length are unaffected; therefore this free-streaming length sets a minimum scale for structure formation.
Cold dark matter – objects with a free-streaming length much smaller than a protogalaxy
Warm dark matter – particles with a free-streaming length similar to a protogalaxy.
Hot dark matter – particles with a free-streaming length much larger than a protogalaxy.
Though a fourth category had been considered early on, called mixed dark matter, it was quickly eliminated (from the 1990s) since the discovery of dark energy.

girasol0821

谢谢楼主，辛苦了

huangkang3039

Sally, 另外一个补充-
关于24题中的海豹题，你后面跟着的一个狗主的解释不太对，容易让人误解。（文章中的FAST,代表的是绝食、禁食的意思，而不是快速的意思）如果理解为快速，全文完全乱套，逻辑混乱，只有作为绝食的意思才能顺通。
你可以添加下附注，关于这篇文章。
文章中说的是海豹和海狮的哺乳策略不同。海狮是在生完崽之后的5-11天不吃东西，用之前储存的脂肪来哺乳。之后的4个月到3年的哺乳期内，他们就会出去觅食了。 而海豹和海狮不一样，生物学家假设海豹整个哺乳期都不用出去觅食。但是最近有个研究表明，有一种海豹H开头的（麻斑海豹）它产崽后6天就出去觅食了。
H海豹这种策略是因为身形小，所以它储存的脂肪19天内就用掉80%了，所以不得不出去觅食。此外，还有另一种海豹（R开头）的，也是身形跟H海狮差不多，也是采用和海狮一样的哺乳期出去觅食的策略。

sally77589

Sally, 另外一个补充-
关于24题中的海豹题，你后面跟着的一个狗主的解释不太对，容易让人误解。（文章中的FAST,代表的是绝食、禁食的意思，而不是快速的意思）如果理解为快速，全文完全乱套，逻辑混乱，只有作为绝食的意思才能顺通。
你可以添加下附注，关于这篇文章。
文章中说的是海豹和海狮的哺乳策略不同。海狮是在生完崽之后的5-11天不吃东西，用之前储存的脂肪来哺乳。之后的4个月到3年的哺乳期内，他们就会出去觅食了。 而海豹和海狮不一样，生物学家假设海豹整个哺乳期都不用出去觅食。但是最近有个研究表明，有一种海豹H开头的（麻斑海豹）它产崽后6天就出去觅食了。
H海豹这种策略是因为身形小，所以它储存的脂肪19天内就用掉80%了，所以不得不出去觅食。此外，还有另一种海豹（R开头）的，也是身形跟H海狮差不多，也是采用和海狮一样的哺乳期出去觅食的策略。

-- by 会员 huangkang3039 (2012/7/29 21:33:05)

好的！感谢~

Addicted潇潇

谢谢小饼~ 爱你们~！