找回密码
 新注册用户
搜索
查看: 6287|回复: 7

[已完成翻译] 我们都是星尘

[复制链接]
发表于 2006-7-29 15:00:17 | 显示全部楼层 |阅读模式
by Amir Alexander
July 21, 2006
原文出自
http://www.planetary.org/program ... erstellar_dust.html

"We are stardust" --Joni Mitchell.

我们是星尘

Light-years from any star or planet, in the vast empty stretches that separate one star from the next, space is not quite as empty as it seems. Even in those dark regions, where nothingness prevails, something, nonetheless, is. It is hard to detect, and easy to miss, but astronomers still know that it's there, because it makes trouble. It gets in the way of our observations of distant objects, distorts what we see of others by absorbing certain wavelengths of radiation, and blurs our view of neighboring stars. When we look towards the center of our galaxy, it gets even worse – an impenetrable screen seems to descend between us and that star-rich region, blocking even the brightest stars from our view. Something is definitely out there in that space between the stars, dense in the center of the galaxy, thinner but noticeable in the outlying regions, always interfering with our orderly observations.

任何一个恒星或行星都在数光年以外,在分割星球间的巨大延伸中,并不是如同想象中的那么空旷。即使在那些黑暗的充斥着虚无的区域也是如此。这很难探测,很容易漏掉,但是天文学家仍然知道它们就在那里,因为它们在制造麻烦。它们处在要观测的遥远物体与我们之间,通过吸收特定波长的辐射扭曲了我们所看到的一些景象,并使邻近我们的星体变得模糊。当我们向银河系的中心看去的时候,情况变得更糟——如同一道难以透过的帷幕落在了我们和那片富星区域之间,阻挡着即使最明亮的恒星进入我们的视野。在那片恒星间的空间中,肯定存在着什么东西,银河中心的密集,外围区域较薄但是明显,总是妨碍我们进行有条理的观察。

Astronomers are a resourceful lot, however, and not much given to brooding over what they might have observed if this troublesome interstellar substance did not get in the way. Instead they focus on the positive, and see what they can learn from the interference itself about this strange substance. And this, it turns out, is quite a lot. First they concluded that this "stuff" is made of tiny grains, because only such particles would reflect and deflect the light in such a way. They also found that the particles affected the different parts of the spectrum of visible light differently – blue light was scattered more than red light, causing objects to appear "redder" than they would otherwise. This meant that the particles were truly miniscule – smaller than the wavelength of visible light, and therefore affecting the shortest wavelengths more than the longer ones. By closely monitoring the precise frequencies of the spectrum that were lost in the passage the passage through empty space, astronomers were actually able to pinpoint the size of different types of these grains, all ranging from less than 1/100th of a micron to 10 microns in size, with each micron representing one millionth of a meter. For comparison, a particle of smoke is about 1/10th of a micron in size. Together, these particles form that most diffuse and insubstantial of substances -- interstellar dust.

天文学家有很多的手段,但是仍然对如果没有挡在途中的讨厌的干扰会观察到什么念念不忘。取而代之的是他们的注意力转向积极的方面,看看能从这些奇怪的干扰物本身学到些什么。这个物质,很明显,非常多。首先他们想到这个物质是微小的颗粒构成的,因为只有这样的微粒能以此种方式反射、偏转光线。他们发现这些微粒对可见光中不同的频谱影响不同——蓝光散射的比红光多,使目标看上去较红。这意味着微粒的确非常小——小于可见光的波长,因此对短波的影响大于长波。通过对穿越真空途中丢失了的光的精细频率的密切监视,天文学家已经基本上可以查明这些不同微粒的大小,大小从小于百分之一微米到十微米之间,一微米表示一米的百万分之一。作为比较,烟中的微粒大约是在十分之一微米大小。聚集在一起,这些微粒形成了大多数弥漫、脆弱的物质——星际尘埃。

For observational astronomers interstellar dust is mostly an inconvenience, but for scientists studying the origins and evolution of the universe they are much much more. In fact, these miniscule grains floating in empty space are responsible for much of the world we see around us. According to current theories, the Big Bang, which occurred around 13 billion years ago, created only the simplest and lightest elements – mostly hydrogen, some helium, and traces of lithium and beryllium. The heavier elements that make up our world were all formed later on – in the cores of burning stars. But how were such elements disseminated throughout the universe, ending up on small rocky planets such as ours? The surprising answer is, through interstellar dust. These insignificant-seeming particles flow through interstellar space, carrying with them the essential components that make stars and planets possible.

对观测天文学家来说星际尘埃通常是一个麻烦,但是对研究宇宙起源和演化的科学家来说它们是非常非常有用的。实际上,这些飘浮在真空中微小的颗粒造就了我们所见的周围世界。根据当前的理论,发生在130亿年前的大爆炸,仅产生了最简单、最轻的元素——多数是氢,一些氦,痕量的锂和铍。那些构成我们这个世界的较重的元素随后在燃烧的恒星核心上以及核心内形成。但是这些元素是如何在宇宙中散布的到处都是,最后终止在我们这个小小的岩石星球上的呢?令人吃惊的回答是:通过星际尘埃。这些看上去无关紧要的微粒漂浮在星际空间,自身携带着使恒星和行星得以产生的不可或缺的成分。

From the Cores of Aging Stars

来自衰老恒星核心

Interstellar dust is formed through several different processes that take place during the lifetime of stars. Our own Sun, for example, is currently about half way through its "main sequence," which is expected to last for another 5 billion years or so. During this stage the Sun "burns" hydrogen in its core, combining hydrogen atoms into helium atoms in a process of nuclear fusion. When this process approaches completion, and a substantial part of the core is composed of helium, the pressure generated by the fusion process in the core diminishes, and the outer layers of the star begin to press in upon the core. This gravitational contraction in turn heats up the core once more, to an even higher degree than before, causing the outer envelopes to heat up and expand. At this point, our familiar Sun will grow to be a Red Giant, encompassing the orbits of Mercury and Venus. The core meanwhile will reach a temperature of 100 million degrees Kelvin, and the helium nuclei will begin fusing into carbon nuclei. At the end of the process a carbon core of the star will be surrounded by a shell where helium is still being fused into carbon, which in turn is surrounded by and envelope where hydrogen is converted into helium. Stars at this stage of their lifespan are known as "Asymptotic Giant Branch" (AGB) stars, and they are highly volatile. Their shells, which apart from hydrogen, helium, and carbon also contain portions of the heavy elements formed in the stellar core, are inherently unstable, and their pulsing creates a withering stellar wind a billion times stronger than the solar wind we know today. In a relatively short time (about 1000 years) the entire shells will be ejected into space, joining the gas and dust in the interstellar medium.

在恒星的一生中会以几种不同的方法形成星际尘埃。举个例子,我们的太阳目前走过了它“主序”阶段的一半,预计这个阶段还会持续大约50亿年。这一时期太阳在它的核心“燃烧”氢,将氢原子通过核聚变结合成氦原子。当这一过程接近完成时,核心的很大一部分由氦组成,核心处由于核聚变产生的压力变小了,同时恒星其他层开始压缩被到核心上。重力坍缩使核心温度升得更高,导致其他壳层升温并膨胀。此刻我们熟悉的太阳将膨胀成为红巨星,会把水星和金星的轨道包含进去。在此期间核心温度会达到1亿K,氦原子核将开始聚变成碳原子核。该过程结束时碳的星核会被一层仍然在进行氦聚变为碳的壳层包围,而在这个氦-碳聚变层的外面还包围着一层由氢-氦聚变层。恒星在它寿命的这一时期被认称为“渐进巨星支”(AGB)星,并且非常的不稳定。它的壳层除了氢层、氦曾和碳层外还有包含一部分产生自恒星核心的重元素,天生的不稳定,它们的脉动产生了一种毁灭性的星风,比我们现在知道的太阳风要强数百万倍。在相对较短的一段时间里(大约1000年)整个壳层将被抛入太空,加入到星际介质的气体和尘埃中。

Most stars are likely to share the life sequence of our Sun. Following a prolonged "main sequence" period they will briefly flower into a "red giant," and shed much of their mass before finally fading into a small and astoundingly dense "white dwarf." But truly heavy stars, more than 8 times as massive as the Sun, have an even more dramatic fate in store. Unlike the Sun, which remains in its main sequence stage for 10 billion years, these giants race through their main sequence stage in a fraction of the time. A star of 15 solar masses, for example, goes through its main sequence stage a thousand times faster than the Sun, converting the entire store of hydrogen in their core into helium in only 10 million years! When this process is complete, the star's core contracts under the gravitational pressure of the outer layers, and heats up to a hundred million degrees. The extreme heat and pressure then initiate a new nuclear reaction in the core – the conversion of helium to carbon. Repeated cycles see the core converted into a series of increasingly heavy elements – neon, magnesium, silicon, sulphur, and eventually – iron and nickel. At this point the cycle of conversion ends: iron, unlike the lighter elements that preceded it, does not release energy when it undergoes nuclear reactions, but absorbs it. For a star this means that an iron core no longer produces the internal pressure needed to counteract the weight of the outer layers of the star, pressing in upon it. Within milliseconds, the star then collapses in upon itself, and when its center can contract no more – it produces a catastrophic explosion. This is a supernova, which when seen from Earth, appears as a bright new star in a place where none (or only a very faint star) appeared to be before. A supernova not only blasts the heavy elements formed in the star out into interstellar space, but also initiates its own nuclear reaction, producing even heavier elements. All of this, in the form of fine grains, becomes the stuff of interstellar dust.

大多数恒星和我们的太阳有着相似的生命序列。在主序阶段停留相当长的一段时期后将短暂的发育成红巨星,并在最终枯萎成为非常致密的白矮星前散失掉大部分的质量。然而那些真正重的恒星,超过8倍太阳质量的,有着一个更加戏剧性的既定命运。和停留在自己主序阶段100亿年的太阳不同,这些巨人在自己的主序阶段奔跑一小部分的时间。举例来说,一个15倍太阳质量的恒星跑过自己的主序期的速度比太阳快一千倍,只用一千万年就将其核心所有的氢转变为氦。当这一过程结束时,恒星的核心在外层的重压下收缩,温度上升到一亿度。在这种极高的温度和压力下核心启动了新的核反应——由氦到碳的转变。重复这种循环核心逐渐被转变成一系列更重的元素——氮、镁、硅、硫、最后是铁和镍。此时转变停了下来:铁不像它前面的轻元素那样经历核反应时会放出能量,相反会吸收能量。对恒星来说这意味着铁核心不再产生用以抵挡外层重量的内部压力。在几毫秒内恒星向内崩溃了,然而此时它的核心已经不能再被压缩——灾难性的爆炸发生了。这就是超新星,从地球上看原本没有星星(或者是一颗很黯淡的星)的地方出现了一个明亮的新星。超新星不仅把恒星内形成的重元素抛入星际空间,而且它本身也会引发核反应产生更重的元素。所有这些以细微颗粒的形式成为星际尘埃的原料。

AGB stars and supernovae of this type (known technically as "type II" supernovae) are two of the most common sources of interstellar dust, though there are others as well. All of them involve the expulsion into space of grains of "heavy" elements formed in the cores of stars. Once they are out floating in the vast emptiness of space, they may join with other dust particles and interstellar gas, and become a swirling cloud of debris. It was precisely such a cloud of gas and dust that condensed to form our Sun and planets, just as similar clouds condensed to form other "second generation" stars. These seemingly insignificant particles of interstellar dust are, in other words, fundamental building blocks of the universe.

这种类型的超新星(学术上称为“II”型超新星)和AGB星是星际尘埃共同的主要来源,虽然还有其他的一些形式。它们将恒星内部形成的重元素微粒抛进太空。一旦这些微粒飘进广袤的太空,它们可能与其他的星际尘埃、气体混合,形成一个旋转的云骸。这正是那个收缩形成太阳和行星的气体和尘埃云,如同类似的收缩成其他“第二代”恒星的尘云。这些看上去不起眼儿的星际尘埃微粒,换句话说,是构建宇宙的基本砖块儿。

The Hunt Begins

狩猎开始了

This being the case, it is hardly surprising that scientists have been eager to get a hold of interstellar dust grains, believing that their study could shed much light on some of the "Big" questions of science: where did we come from, how did our world become what it is, and where is it heading? Unfortunately, until the spacecraft Stardust returned with its samples on January 15 of this year, it was not clear where any could be found. In fact, it was not even clear how any particle, if found, could even be identified as a grain interstellar dust.

事情源自科学家一直以来渴求得到星际尘埃这一事实,相信通过他们的研究将使一些“大”的科学问题如:我们来自何处,世界是怎样变成它现在的这个样子的,以及它将向何处发展?变得更加明朗。不幸的是直到今年1月15日“星尘”号飞船带着样品返回,也不能确定会发现什么。实际上,还不清楚能有多少颗粒,如果找到的话,可以被确认为是星际尘埃。

They did have one good lead to go on: when interstellar dust grains form in the cores of stars and are then ejected into space, they carry with them the signature of the event that produced them. Depending on the nature of this event, the proportions of the different isotopes of any given elements are somewhat different. Isotopes are different varieties of the same type of atom, all completely identical in their chemical behavior, but differing slightly in their atomic weight. The most common isotope of oxygen, for example, has an atomic weight of 16, but there are also rarer isotopes with weights of 17 and 18, caused by additional neutrons in their nuclei. According to existing models, the proportions between the different isotopes in a dust grain formed in a supernova will differ from the proportions of the same isotopes in a grain formed in an AGB star, which in turn will differ from isotopic proportions in grains formed in other ways. This, scientists reasoned, should help in identifying these elusive particles if they are, in some way, located.

科学家们确实寄希望于:当星际尘埃从恒星核心形成以及随后被抛入太空,携带着它们诞生时的信息。基于这种特性,特定元素的同位素比例会有些许不同。同位素是同一原子的不同品种,具有完全吸纳共同的化学特性,只是它们的原子核重量有点不同。例如很常见的同位素氧,原子重量是16,但是还有更为稀少的重量为17和18的同位素,这是因为它们的原子核中有额外的中子。根据现有模型,产生自超新星的尘埃颗粒的同位素比例会与产生自AGB星的尘埃有所不同,而且以其他途径产生的颗粒其同位素比例也会不同。如果能以某种方式将它们的位置确定下来,这将有助于鉴别这些难以捉摸的颗粒。

As long as scientists had no good way to measure isotopic proportions, the whole question was, well, "academic." But in the 1950s the first sophisticated mass spectrometers were developed, capable of measuring isotopes in small samples. At first, scientists set their sites on meteorites, looking to see if these object from outer space had their own unique isotopic signature. It quickly became clear, however, that the isotopic composition of meteorites differed not at all from that of the Earth itself. These solar system objects, it seemed, came from the same atomic "soup" that gave birth to the Sun, the Earth, and the nine familiar planets. Far from yielding unusual isotopic distributions, the asteroids provided powerful evidence that the entire solar system was formed of a single relatively homogenous cloud of gas and dust billions of years ago.

长久以来科学家没有很好的方法测量同位素的比例,所有的问题都是“理论上的”。但是上世纪50年代发展出的精细质谱仪能够测定少量样品中的同位素。科学家首先瞄准了陨石,看看这些来自外太空的物体是否有独特的同位素特征。然而事情很快清楚了,陨石中的同位素比例与地球自身没有什么不同。看起来太阳系的物体都是来自赋予太阳、地球和九大行星生命的同一“原子汤”。非但没有屈从于不寻常的同位素分布,陨石提供了强有力的证据显示整个太阳系诞生自数十亿年前的一块同源尘埃和气体云。

Burning Down the Haystack

洗尽铅华

For the next 30 years or so, despite intense effort, nobody was able to identify individual grains of ancient interstellar dust. But in the 1980's scientists at the University of Chicago, led by Ed Anders, and at Washington University in Saint Louis, led by Ernst Zinner, did finally manage to extract grains of highly unusual isotopic composition from meteorites. They used highly corrosive chemical agents to isolate grains that seemed like they could not possibly have come from the relatively homogenous dusty cloud that gave rise to the solar system. Composed of micro diamonds, aluminum oxide, and silicon carbide, the isotopic distribution of these grains bore the telltale marks of their birth: ancient supernovas and red giant stars, that shone brightly and then flickered out, billions of years ago, before the birth of the solar system.

在随后的大约30年里,尽管非常的努力也还是没有人能够鉴别出单独的原始星际尘埃。但是在八几年,由 Ed Anders 领导的芝加哥大学和 Ernst Zinner 领导的华盛顿大学的科学家们,最终从陨石中提取出有着极不寻常的同位素成分的颗粒。他们用高度腐蚀性的化学制剂分离出被认为是不可能来自与我们的太阳系同源相关的尘云。由微金刚石、铝氧化物、碳化硅组成的这些微粒的同位素分布透露出它们的诞生:那些数十亿年前,在太阳系尚未诞生时,曾经闪耀并最终熄灭的古老超新星和红巨星。

The work of Zinner, Anders and their colleagues was a landmark in the study of interstellar dust particles. For the first time, grains from distant stars were available for study by scientists on Earth, and could be compared with the solar system element scientists know so well. Nevertheless, there were serious limitations that had to be kept in mind when studying these unusual dust grains. First there was the matter of the process used to extract the grains from the meteorites in which they were found. The procedure involved the use of extremely corrosive chemical agents, which destroyed most of the rock in order to preserve the interstellar particles within. The process is so extreme that Anders referred to it as "burning down the haystack to find the needle." It is quite possible that just as the chemicals corrode the meteorite, they also destroy some interstellar grains that are not recognized as such. A second, related, problem is that in all likelihood the samples collected in this manner are not at all representative of "normal" interstellar dust particles, and are, in fact, highly unusual. This is because the procedure only recognizes grains as being of interstellar origin when their isotopic proportions are extremely different from the proportions in Earthly minerals. If the proportions in an interstellar dust particle are only moderately different, or actually similar, to what one finds on Earth, this method would never identify the particle as being a grain of interstellar dust. The end result is that by definition, the samples produced through Zinner's chemical process are very atypical, and highly skewed. The only way to obtain a true and unbiased sample of interstellar dust particles is to go to where they are – in space – and collect them there.

Zinner、Ander 和它们的同事所作的工作是星际尘埃微粒研究中的一块里程碑。这使得科学家第一次在地球上研究来自遥远恒星的微粒成为可能,并能够与科学家们所熟知的太阳系成分进行比较。然而在研究这些不寻常的尘埃颗粒时头脑中必须要有严肃的限制。首先是从发现它们的陨石中将其提取出来的方法存在问题。这个过程涉及使用具有强腐蚀性的化学制剂,制剂摧毁了大部分的岩石以便保护在石头内部的星际颗粒。这个方法太极端了以至于 Ander 把它比作“为寻找一根针烧掉整个草堆”。这一过程很可能像腐蚀掉陨石一样会摧毁一些尚未被认识的星际颗粒。其次,与之相关的问题是所有以这种方式收集到的样本不能代表全部的“常规”星际尘埃,实际上它们很不寻常。因为这一过程仅仅把那些同位素比例与地球物质差别很大的颗粒鉴别为源自星际。如果在地球上找到的一个星际尘埃的同位素比例只是稍有不同或者非常相近,这种方法将根本无法把它鉴别为星际尘埃。最终的结果限定了通过 Zinner 的化学处理方法得到的颗粒样本并非是典型的,在统计学上是不均匀的。获得一个真实没有偏差的星际尘埃样本的唯一方法就是到太空去收集。

Pristine particles of Stardust

星尘号的原始颗粒

That is precisely what Stardust did. Two previous missions, Ulysses and Galileo, had already detected the flow of dust particles into the solar system. Scientists could tell it came from interstellar space because it was not affected by the presence of any planet, and because it flowed from precisely the same direction as neutral interstellar gas, which had been detected before. It was, in other words, a stream of interstellar dust flowing right at our doorstep, and Stardust was sent out to collect. On two occasions during its 7 billion mile journey, between February and May of 2000 and again from August to December of 2002, Stardust passed through the dust stream and spread out its collector to the interstellar flow. The stream is so thin, however, that scientists believe that even with seven months of exposure, Stardust probably captured only a few dozen grains of interstellar dust.

这正是星尘号所作的工作。先前的两个任务,尤利西斯和伽利略,已经探测到飘进太阳系的尘埃流。科学家能断定它来自星际空间是因为它没有受到任何行星的影响,并且和以前探测到的中性星际气体来自同一方向。换句话说一股星际尘埃的洪流正从我们门前流过,星尘号被派去进行采集。在它7亿英里的旅程中的两个阶段,2000年2月至5月以及2002年8月至12月,星尘号穿越了这股尘埃流并对着尘埃流展开了收集器。尘埃流实在太稀薄了,以至于科学家们认为即使在暴露其中的这7个月时间里,星尘号可能仅仅捕获了几十个星际尘埃的颗粒。

But this, really, is all that scientists need. With a pristine and unbiased sample of interstellar dust they can truly find out if and by how much the elements of our own world differ from others throughout the galaxy. They can study these relatively recent building blocks of the universe, and compare them to those ancient particles frozen in time for the last 4.5 billion years – since the birth of the solar system. Has the galaxy changed? Is it evolving in a particular direction?  Or, to put it in a less scientific but more evocative way – where did we come from and where are we going? The precious particles on Stardust do not have all the answers to these eternal questions. But, scientists believe, they may well provide us with some important clues.

但这些正是科学家们需要的。通过这些原始的无偏见的星际尘埃样品,人们能真正找出究竟我们的太阳系同银河中的其它星球是否有元素差异以及相差多少。科学家们得以研究这些相对较新的宇宙砖块,并和那些古老的——自太阳系诞生以来就一直保持原貌的颗粒进行比较。银河系有变化么?它是否在朝独特的方向演化?或者从更具启发性的方式思考——我们来自何处又将去向何方?星尘号上的珍宝并不能回答所有这些永恒的问题。但是科学家相信它们将会提供给我们一些重要的线索。



=====================
欢迎观赏

[ Last edited by Rojer on 2006-7-30 at 14:48 ]

评分

参与人数 2基本分 +200 维基拼图 +100 收起 理由
BiscuiT + 200 + 50
霊烏路 空 + 50

查看全部评分

回复

使用道具 举报

发表于 2006-7-29 21:10:40 | 显示全部楼层
楼主辛苦了,非常好的一篇文章,周一我就把她转到我们服务器上去。
回复

使用道具 举报

发表于 2006-8-10 19:26:34 | 显示全部楼层
本页文章已转至 http://www.equn.com/stardust/interstellar_dust.html ,为了保持 stardust 中文站内其他翻译自“行星协会”的文章结构的一致性,所以采用第一版网站外观。站点地图随后更新。
回复

使用道具 举报

 楼主| 发表于 2006-8-10 23:51:47 | 显示全部楼层
大仙辛苦了!
回复

使用道具 举报

发表于 2006-8-11 22:22:54 | 显示全部楼层
不辛苦不辛苦,我就扮演了一下剪刀手的角色而已。还要继续麻烦 Rojer 把页面里的几段图片说明翻译一下,谢谢!
回复

使用道具 举报

 楼主| 发表于 2006-8-12 11:12:39 | 显示全部楼层
The Milky Way

A side view of the Milky Way galaxy. The central bulge of the galaxy is blocked to observation in the visible wavelengths, due to the interference by interstellar dust. It can, however, be observed at the longer, infrared wavelengths.
银河系
从侧面看银河系。星系中心突起的部分因受星际尘埃的阻挡无法用可见光观察。然而可以用波长较长的红外线观察。


A Cluster of Supergiants

This group of supergiant stars, each about 20 solar masses, reside in a massive star cluster of our galaxy about 18,900 light-years away. The stars are at the end of their core-burning phase, and are due to explode into supernovae. This false-color image was taken with the Caltech-based Two Micron All Sky Survey (2MASS).
一个超巨星群
这一组超巨星位于银河系18900光年远的一个大质量恒星群中,每一个都有20倍太阳质量。这些恒星都处在核心燃烧阶段末期,即将爆炸成为超新星。这幅伪彩色图片是近红外全天搜索计划(Two Micron All Sky Survey)的加州理工学院方面拍摄的。



The Dusty Remains of a Supernova

This supernova, named E0102, is in the Large Magellanic Cloud, a satellite galaxy to the Milky Way about 200,000 light-years away. The image shows the hot bubble of dust surrounding the remainder of the star, spreading towards interstellar space. The dust particles carry with them heavy elements forged in the core of the star.
一个超新星的尘埃残骸
这个名为 E0102 的超新星位于银河系的一个伴星系大麦哲伦星云(约20万光年远)中。图像显示出残骸周围的热尘埃泡,正在向星际空间扩展。尘埃携带着在恒星核心铸造出的重元素。
回复

使用道具 举报

发表于 2006-8-12 13:47:58 | 显示全部楼层
谢谢,已更新 http://www.equn.com/stardust/interstellar_dust.html

另外,请楼主在 Stardust@home 讨论区放一个置顶帖,简要的介绍一下项目主旨,然后大概的写写参与过程,然后给出供参考的帖子链接。
回复

使用道具 举报

发表于 2006-8-18 21:37:35 | 显示全部楼层
好文!值得收藏。
回复

使用道具 举报

您需要登录后才可以回帖 登录 | 新注册用户

本版积分规则

论坛官方淘宝店开业啦~
欢迎大家多多支持基金会~

Archiver|手机版|小黑屋|中国分布式计算总站 ( 沪ICP备05042587号 )

GMT+8, 2024-3-29 18:11

Powered by Discuz! X3.5

© 2001-2024 Discuz! Team.

快速回复 返回顶部 返回列表