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2、求一个星盘的解释：用什么软件能获得。怎么获得解释说明，如何判断生辰天宫图的其你部分很有利与否？
时空中点盘 火星8宫
《时间简史08｜宇宙的起源和命运1（中英文）》
In an attempt to find a model of the universe in which many different initial configurations could have evolved tosomething like the present universe, a scientist at the Massachusetts Institute of Technology, Alan Guth, suggestedthat the early universe might have gone through a period of very rapid expansion. This expansion is said to be“inflationary,” meaning that the universe at one time expanded at an increasing rate rather than the decreasing ratethat it does today. According to Guth, the radius of the universe increased by a million million million million million (1with thirty zeros after it) times in only a tiny fraction of a second.
为了试图寻找一个能从许多不同的初始结构演化到象现在这样的宇宙的宇宙模型，麻省理工xué院的科学家阿伦·固斯提出，早期宇宙可能存在过一个非常快速膨胀的时期。这种膨胀叫做“暴涨”，意指宇宙在一段时间里，不像现在这样以减少的、而是以增加的速率膨胀。按照固斯理论，在远远小于1秒的时间里，宇宙的半径增大了100万亿亿亿（1后面跟30个0）倍。
Guth suggested that the universe started out from the big bang in a very hot, but rather chaotic, state. These hightemperatures would have meant that the particles in the universe would be moving very fast and would have highenergies. As we discussed earlier, one would expect that at such high temperatures the strong and weak nuclearforces and the electromagnetic force would all be unified into a single force. As the universe expanded, it would cool,and particle energies would go down. Eventually there would be what is called a phase transition and the symmetrybetween the forces would be broken: the strong force would become different from the weak and electromagneticforces. One common example of a phase transition is the freezing of water when you cool it down. Liquid water issymmetrical, the same at every point and in every direction. However, when ice crystals form, they will have definitepositions and will be lined up in some direction. This breaks water’s symmetry.
固斯提出，宇宙是以一个非常热而且相当紊乱的状态从大爆炸开始的。这些高温表明宇宙中的粒子运动得非常快并具有高能量。正如早先我们讨论的，人们预料在这么高的温度下，强和弱核力及电磁力都被统一成一个dān独的力。当宇宙膨胀时它会变冷，粒子能量下降。最后出现了所谓的相变，并且力之间的对称性被破坏了：强力变得和弱力以及电磁力不同。相变的一个普通的例子是，当水降温时会冻结成冰。液态水是对称的，它在任何一点和任何方向上都是相同的。rán而，当冰晶体形成时，它们有确定的位置，并在某一方向上整齐排列，这就破坏了水的对称。
In the case of water, if one is careful, one can “supercool” it: that is, one can reduce the temperature below thefreezing point (OºC) without ice forming. Guth suggested that the universe might behave in a similar way: thetemperature might drop below the critical value without the symmetry between the forces being broken. If thishappened, the universe would be in an unstable state, with more energy than if the symmetry had been broken. Thisspecial extra energy can be shown to have an antigravitational effect: it would have acted just like the cosmologicalconstant that Einstein introduced into general relativity when he was trying to construct a static model of theuniverse. Since the universe would already be expanding just as in the hot big bang model, the repulsive effect ofthis cosmological constant would therefore have made the universe expand at an ever-increasing rate. Even inregions where there were more matter particles than average, the gravitational attraction of the matter would havebeen outweighed by the repulsion of the effective cosmological constant. Thus these regions would also expand inan accelerating inflationary manner. As they expanded and the matter particles got farther apart, one would be leftwith an expanding universe that contained hardly any particles and was still in the supercooled state. Anyirregularities in the universe would simply have been smoothed out by the expansion, as the wrinkles in a balloon aresmoothed away when you blow it up. Thus the present smooth and uniform state of the universe could have evolvedfrom many different non-uniform initial states.
处理水的时候，只要你足够小心，就能使之“过冷”，也就是可以将温度降低到冰点（0℃）以下而不结bīng。固斯认为，宇宙的行为也很相似：宇宙温度可以低到临界值以下，而没有使不同的力之间的对称受到破坏。如果发生这种情形，宇宙就处于一个不稳定状态，其能量比对称破缺时更大。这特殊的额外能量呈现出反引力的效应：其作用如同一个宇宙常数。宇宙常数是当爱因斯坦在试图建立一个稳定的宇宙模型时，引进广义相对论之中去的。由于宇宙已经像大爆炸模型那样膨胀，所以这宇宙常数的排斥效应使得宇宙以不断增加的速度膨胀，即使在一些物质粒子比平均数多的区域，这一有效宇宙常数的排斥作用超过了物质的引力吸引作用。这样，这些区域也以加速暴涨的形式而膨胀。当它们膨胀时，物质粒子越分越开，留下了一个几乎不包含任何粒子，并仍然处于过冷状态的膨胀的宇宙。宇宙中的任何不规则性都被这膨胀抹平，正如当你吹胀气球时，它上面的皱纹就被抹平了。所以，宇宙现在光滑一致的状态，可以是从许多不同的非一致的初始状态演化而来。
In such a universe, in which the expansion was accelerated by a cosmological constant rather than slowed down bythe gravitational attraction of matter, there would be enough time for light to travel from one region to another in theearly universe. This could provide a solution to the problem, raised earlier, of why different regions in the earlyuniverse have the same properties. Moreover, the rate of expansion of the universe would automatically becomevery close to the critical rate determined by the energy density of the universe. This could then explain why the rateof expansion is still so close to the critical rate, without having to assume that the initial rate of expansion of theuniverse was very carefully chosen.
在这样一个其膨胀由宇宙常数加速、而不由物质的引力吸引使之减慢的宇宙中，早期宇宙中的光线就有足够的时间从一个地方传到另一个地方。这就解答了早先提出的，为何在早期宇宙中的不同区域具有同样性质的问题。不但如此，宇宙的膨胀率也自动变得非常接近于由宇zhòu的能量密度决定的临界值。这样，不必去假设宇宙初始膨胀率曾被非常仔细地选择过，就能解释为何现在的膨胀率仍然是如此地接近于临界值。
The idea of inflation could also explain why there is so much matter in the universe. There are something like tenmillion million million million million million million million million million million million million million (1 with eightyzeros after it) particles in the region of the universe that we can observe. Where did they all come from? The answeris that, in quantum theory, particles can be created out of energy in the form of particle/antiparticle pairs. But that justraises the question of where the energy came from. The answer is that the total energy of the universe is exactlyzero. The matter in the universe is made out of positive energy. However, the matter is all attracting itself by gravity.Two pieces of matter that are close to each other have less energy than the same two pieces a long way apart,because you have to expend energy to separate them against the gravitational force that is pulling them together.Thus, in a sense, the gravitational field has negative energy. In the case of a universe that is approximately uniformin space, one can show that this negative gravitational energy exactly cancels the positive energy represented by thematter. So the total energy of the universe is zero.
暴涨的思想还能解释为何宇宙存在这么多物质。在我们能观察到的宇宙里大体有1亿亿亿亿亿亿亿亿亿亿（1后面跟80个0）个粒子。它们从何而来？答案是，在量子理论中，粒子可以从粒子/反粒子对的形式由能量中创生出来。但这只不过引起了能量从何而来的问题。答案是，宇宙的总néng量刚好是零。宇宙的物质是由正能量构成的；然而，所有物质都由引力互相吸引。两块互相靠近的物质比两块分得很开的物质具有更少的能量，因为你必须消耗能量去克服把它们拉在一起的引力而将其分开。这样，在一定意义上，引力场具有负能量。在空间上大体一致的宇宙的情形中，人们可以证明，这个负的引力néng刚好抵消了物质所代表的正能量，所以宇宙的总能量为零。
Now twice zero is also zero. Thus the universe can double the amount of positive matter energy and also double thenegative gravitational energy without violation of the conservation of energy. This does not happen in the normalexpansion of the universe in which the matter energy density goes down as the universe gets bigger. It does happen,however, in the inflationary expansion because the energy density of the supercooled state remains constant whilethe universe expands: when the universe doubles in size, the positive matter energy and the negative gravitationalenergy both double, so the total energy remains zero. During the inflationary phase, the universe increases its sizeby a very large amount. Thus the total amount of energy available to make particles becomes very large. As Guthhas remarked, “It is said that there’s no such thing as a free lunch. But the universe is the ultimate free lunch.”
零的两倍仍为零。这样宇宙可以同时将其正的物质能和负的引力能加倍，而不破坏其能量的守恒。在宇宙的正常膨胀时，这并没有发生。这时当宇宙变大时，物质能量密度下降。然而，这种情形确实发生于暴涨时期。因为宇宙膨胀时，过冷态的能量密度保持不变：当宇宙体积加倍时，正物质能和负引力能都加倍，总能量保持为零。在暴涨相，宇宙的尺度增大了一个非常大的倍数。这样，可用以制造粒子的总能量变得非常大。正如固斯所说的：“都说没有免费午餐这件事，但是宇宙是最彻底的免费午餐。”
The universe is not expanding in an inflationary way today. Thus there has to be some mechanism that wouldeliminate the very large effective cosmological constant and so change the rate of expansion from an acceleratedone to one that is slowed down by gravity, as we have today. In the inflationary expansion one might expect thateventually the symmetry between the forces would be broken, just as super-cooled water always freezes in the end.The extra energy of the unbroken symmetry state would then be released and would reheat the universe to atemperature just below the critical temperature for symmetry between the forces. The universe would then go on toexpand and cool just like the hot big bang model, but there would now be an explanation of why the universe wasexpanding at exactly the critical rate and why different regions had the same temperature.
今天宇宙不是以暴涨的方式膨胀。这样，必须有一种机制，它可以消去这一非常大的有效宇宙常数，从而使膨胀率从加速的状态，改变为正如同今天这样由引力减慢下的样子。人们可以预料，在宇宙暴涨时不同力之间的对称最终会被破坏，正如过冷的水最终会凝固一样。这样，未破缺的对称态的额外能量就会释放，并将宇宙重新加热到刚好低于使不同力对称的临界温度。以后，宇宙就以标准的大爆炸模式继续膨胀并变冷。但是，现在找到了何以宇宙刚好以临界速率膨胀，并在不同的区域具有相同温度的解释。
In Guth’s original proposal the phase transition was supposed to occur suddenly, rather like the appearance of icecrystals in very cold water. The idea was that “bubbles” of the new phase of broken symmetry would have formed inthe old phase, like bubbles of steam surrounded by boiling water. The bubbles were supposed to expand and meetup with each other until the whole universe was in the new phase. The trouble was, as I and several other peoplepointed out, that the universe was expanding so fast that even if the bubbles grew at the speed of light, they wouldbe moving away from each other and so could not join up. The universe would be left in a very non-uniform state,with some regions still having symmetry between the different forces. Such a model of the universe would notcorrespond to what we see.
在固斯的原先设想中，有点像在非常冷的水中出现冰晶体，相变是突然发生的。其想法是，正如同沸腾的水围绕着蒸汽泡，新的对称破缺相的“泡泡”在原有的对称相中形成。泡泡膨胀并互相碰撞，直到整个宇宙变成新相。麻烦在于，正如同我和其他几个人所指出的，宇宙膨胀得如此之快，甚至即使泡泡以光速涨大，它们也要互相分离，并因此不能合并在一起。结果宇宙变成一种非常不一致的状态，有些区域仍具有不同力之间的对称。这样的模型跟我们所观察到的宇宙并不吻合。
the inflationary model and its problems at the Sternberg Astronomical Institute. Before this, I had got someone elseto give my lectures for me, because most people could not understand my voice. But there was not time to preparethis seminar, so I gave it myself, with one of my graduate students repeating my words. It worked well, and gave memuch more contact with my audience. In the audience was a young Russian, Andrei Linde, from the LebedevInstitute in Moscow. He said that the difficulty with the bubbles not joining up could be avoided if the bubbles were sobig that our region of the universe is all contained inside a single bubble. In order for this to work, the change fromsymmetry to broken symmetry must have taken place very slowly inside the bubble, but this is quite possibleaccording to grand unified theories. Linde’s idea of a slow breaking of symmetry was very good, but I later realizedthat his bubbles would have to have been bigger than the size of the universe at the time! I showed that instead thesymmetry would have broken everywhere at the same time, rather than just inside bubbles. This would lead to auniform universe, as we observe. I was very excited by this idea and discussed it with one of my students, Ian Moss.As a friend of Linde’s, I was rather embarrassed, however, when I was later sent his paper by a scientific journal andasked whether it was suitable for publication. I replied that there was this flaw about the bubbles being bigger thanthe universe, but that the basic idea of a slow breaking of symmetry was very good. I recommended that the paper ¿published as it was because it would take Linde several months to correct it, since anything he sent to the Westwould have to be passed by Soviet censorship, which was neither very skillful nor very quick with scientific papers.Instead, I wrote a short paper with Ian Moss in the same journal in which we pointed out this problem with the bubbleand showed how it could be resolved.
1981年10月，我去莫斯科参加量子引lì的会议。会后，我在斯特堡天文研究所做了一个有关暴涨模型和它的问题的讲演。听众席中有一年轻的苏联人——莫斯科列别提夫研究所的安德雷·林德——他讲，如果泡泡是如此之大，以至于我们宇宙的区域被整个地包含在一个单独的泡泡之中，则可以避免泡泡不能合并在一起的困难。为了使这个行得通，从对称相向对称破缺相的改变必须在泡泡中进行得非常慢，而按照大统一理论这是相当可能的。林德的缓慢对称破缺思想是非常好的，但过后我意识到，他的泡泡在那一时刻必须比宇宙的尺度还要大！我指出，那时对称不仅仅在泡泡里，而且在所有的地方同时被破坏。这会导致一个正如我们所观察到的一致的宇宙。我被这个思想弄dé非常激动，并和我的一个学生因·莫斯讨论。然而，当我后来收到一个科学杂志社寄来的林德的论文，征求是否可以发表时，作为他的朋友，我感到相当难为情。我回答说，这里有一个关于泡泡比宇宙还大的瑕疵，但是里面关于缓慢对称破缺的基本思想是非常好的。我建议将此论文照原样发表。因为林德要花几个月时间去改正它，并且他寄到西方的任何东西都要通过苏联的审查，这种对于科学论文的审查既无技巧可言又很缓慢。我和因·莫斯便越俎代庖，为同一杂志写了一篇短文。我们在该文中指出这泡泡的问题，并提出如何将其解决。
The day after I got back from Moscow I set out for Philadelphia, where I was due to receive a medal from theFranklin Institute. My secretary, Judy Fella, had used her not inconsiderable charm to persuade British Airways togive herself and me free seats on a Concorde as a publicity venture. However, I .was held up on my way to theairport by heavy rain and I missed the plane. Nevertheless, I got to Philadelphia in the end and received my medal. Iwas then asked to give a seminar on the inflationary universe at Drexel University in Philadelphia. I gave the sameseminar about the problems of the inflationary universe, just as in Moscow.
我从莫斯科返回的第二天，即去费城接受富兰克林研究所的奖章。我的秘书朱迪·费拉以其不差的魅力说服了英guó航空公司向她和我免费提供协和式飞机的宣传旅行座席。然而，在去机场的路上被大雨耽搁，我没赶上航班。尽管如此，我最终还是到了费城并得到奖章。之后，应邀作了关于暴涨宇宙的讲演。正如在莫斯科那样，我用大部分时间讲授关于暴涨模型的问题。
A very similar idea to Linde’s was put forth independently a few months later by Paul Steinhardt and AndreasAlbrecht of the University of Pennsylvania. They are now given joint credit with Linde for what is called “the newinflationary model,” based on the idea of a slow breaking of symmetry. (The old inflationary model was Guth’soriginal suggestion of fast symmetry breaking with the formation of bubbles.)
几个月之后，宾州大学的保罗·斯特恩哈特和安德鲁斯·阿尔伯勒希特独立地提出和林德非常相似的思想。现在他们和林德分享以缓慢对称破缺的思想为基础的所谓“新暴胀模型” 的荣誉。（旧的暴胀模型是指固斯关于形成泡泡后快速对称破缺的原始设想。）
The new inflationary model was a good attempt to explain why the universe is the way it is. However, I and severalother people showed that, at least in its original form, it predicted much greater variations in the temperature of themicrowave background radiation than are observed. Later work has also cast doubt on whether there could be aphase transition in the very early universe of the kind required. In my personal opinion, the new inflationary model isnow dead as a scientific theory, although a lot of people do not seem to have heard of its demise and are still writingpapers as if it were viable. A better model, called the chaotic inflationary model, was put forward by Linde in 1983. Inthis there is no phase transition or supercooling. Instead, there is a spin 0 field, which, because of quantumfluctuations, would have large values in some regions of the early universe. The energy of the field in those regionswould behave like a cosmological constant. It would have a repulsive gravitational effect, and thus make thoseregions expand in an inflationary manner. As they expanded, the energy of the field in them would slowly decreaseuntil the inflationary expansion changed to an expansion like that in the hot big bang model. One of these regionswould become what we now see as the observable universe. This model has all the advantages of the earlierinflationary models, but it does not depend on a dubious phase transition, and it can moreover give a reasonable sizefor the fluctuations in the temperature of the microwave background that agrees with observation.
新暴涨模型是一个好的尝试，它能解释宇宙为何是这种样子。然而我和其他几个人指出，至少在它原先的形式，它预言的微波背景辐射的温度起伏bǐ所观察到的情形要大得多。后来的工作还对极早期宇宙中是否存在这类所需要的相变提出怀疑。我个人的意见是，现在新暴涨模型作为一个科学理论是气数已尽。虽然有很多人似乎没有听进它的死讯，还jì续写文章，好像那理论还有生命力。林德在1983年提出了一个更好的所谓紊乱暴涨模型。这里没有相变和过冷，而代之以存在一个自旋为0的场，由于它的量子涨落，在早期宇宙的某些区域有大的场量。在那些区域中，场的能量起到宇宙常数的zuò用，它具有排斥的引力效应，因此使得zhè些区域以暴涨的形式膨胀。当它们膨胀时，它们中的场的能量慢慢地减小，直到暴涨改变到犹如热大爆炸模型中的膨胀时为止。这些区域之一就成为我们看到的宇宙。这个模型具有早先暴涨模型的所有优点，但它不是取决于使人生疑的相变，并且还能给出微波背景辐射的温度起伏，其幅度与观测相符合。
This work on inflationary models showed that the present state of the universe could have arisen from quite a largenumber of different initial configurations. This is important, because it shows that the initial state of the part of theuniverse that we inhabit did not have to be chosen with great care. So we may, if we wish, use the weak anthropicprinciple to explain why the universe looks the way it does now. It cannot be the case, however, that every initialconfiguration would have led to a universe like the one we observe. One can show this by considering a verydifferent state for the universe at the present time, say, a very lumpy and irregular one. One could use the laws ofscience to evolve the universe back in time to determine its configuration at earlier times. According to the singularitytheorems of classical general relativity, there would still have been a big bang singularity. If you evolve such auniverse forward in time according to the laws of science, you will end up with the lumpy and irregular state youstarted with. Thus there must have been initial configurations that would not have given rise to a universe like theone we see today. So even the inflationary model does not tell us why the initial configuration was not such as toproduce something very different from what we observe. Must we turn to the anthropic principle for an explanation?Was it all just a lucky chance? That would seem a counsel of despair, a negation of all our hopes of understandingthe underlying order of the universe.
暴涨模型的研究指出：宇宙现在的状态可以从相当大量的不同初始结构引起的。这是重要的，因为它表明不必非常细心地选取我们居住的那部份宇宙区域的初始状态。所以，如果愿意的话，我们可以利用弱人择原理解释宇宙为何是这个样子。然而，绝不是任何一种初始结构都会产生像我们所观察到的宇宙。这一点很容易说明，考虑现在宇宙处于一个非常不同的态，例如一个非常成团的、非常无规则的态，人们可以利用科学定律，在时间上将其演化回去，以确定宇宙在更早时刻的结构。按照经典广义相对论的奇点定理，仍然存在一个大爆炸奇点。如果你在时间前进方向上按照科学定律演化这样的宇宙，你就会得到你一开始给定的那个成团的无规则的态。这样，必定存在不会产生我们今天所观察到的宇宙的初始结构。所以，就连暴涨模型也没有告诉我们，为何初始结构不是那种产生和我们观测到的非常不同的宇宙的某种态。我们是否应该转去应用人择原理以求解释呢？难道所有这一切仅仅是因为好运气？看来，这只是无望的遁词，是对我们理解宇宙内在秩序的所有希望的否定。
In order to predict how the universe should have started off, one needs laws that hold at the beginning of time. If theclassical theory of general relativity was correct, the singularity theorems that Roger Penrose and I proved show thatthe beginning of time would have been a point of infinite density and infinite curvature of space-time. All the knownlaws of science would break down at such a point. One might suppose that there were new laws that held atsingularities, but it would be very difficult even to formulate such laws at such badly behaved points, and we wouldhave no guide from observations as to what those laws might be. However, what the singularity theorems reallyindicate is that the gravitational field becomes so strong that quantum gravitational effects become important:classical theory is no longer a good description of the universe. So one has to use a quantum theory of gravity todiscuss the very early stages of the universe. As we shall see, it is possible in the quantum theory for the ordinarylaws of science to hold everywhere, including at the beginning of time: it is not necessary to postulate new laws forsingularities, because there need not be any singularities in the quantum theory.
为了预言宇宙应该是如何开始的，人们需要在时间开端处有效的定律。罗杰·彭罗斯和我证明的奇点定理指出，如果广义相对论的经典理论是正确的，则时间的开端是具有无限密度和无限空间——时间曲率的一点，在这一点上所有已知的科学定律都失效。人们可以设想存在在奇点处成立的新定律，但是在如此不守规矩的点处，甚至连表述这样的定律都是非常困难的，而且从观察中我们没有得到关于这些定律应是什么样子的任何提示。然而，奇点定理真正表明的是，该处引力场变得如此之强，以至于量子引力效应变得重要：经典理论不再能很好地描述宇宙。所以，人们必须用量子引力论去讨论宇宙的极早期阶段。我们将会看到，在量子力学中，通常的科学定律有可能在任何地方都有效，包括时间开端这一点在内：不必针对奇点提出新的定律，因为在量子理论中不须有任何奇点。
We don’t yet have a complete and consistent theory that combines quantum mechanics and gravity. However, weare fairly certain of some features that such a unified theory should have. One is that it should incorporateFeynman’s proposal to formulate quantum theory in terms of a sum over histories. In this approach, a particle doesnot have just a single history, as it would in a classical theory. Instead, it is supposed to follow every possible path inspace-time, and with each of these histories there are associated a couple of numbers, one represent-ing the size ofa wave and the other representing its position in the cycle (its phase). The probability that the particle, say, passesthrough some particular point is found by adding up the waves associated with every possible history that passesthrough that point. When one actually tries to perform these sums, however, one runs into severe technicalproblems. The only way around these is the following peculiar prescription: one must add up the waves for particlehistories that are not in the “real” time that you and I experience but take place in what is called imaginary time.Imaginary time may sound like science fiction but it is in fact a well-defined mathematical concept. If we take anyordinary (or “real”) number and multiply it by itself, the result is a positive number. (For example, 2 times 2 is 4, butso is – 2 times – 2.) There are, however, special numbers (called imaginary numbers) that give negative numberswhen multiplied by themselves. (The one called i, when multiplied by itself, gives – 1, 2i multiplied by itself gives – 4,and so on.)
我们仍然没有一套完整而协调的理论，它将量子力学和引力结合在一起。然而，我们相当清楚这样一套统一理论所应该具有的某些特征。其中一个就是它必须和费因曼提出的按照对历史求和的量子力学表述相一致。在这种方法里，一个粒子不像在经典理论中那样，不仅只有一个历史。相反的，它被认为是通过空间——时间里的每一可能的路径，每一条途径有一对相关的数，一个代表波的幅度，另一个代表它的相位。粒子通过一指定点的概率是将通过此点的所有可能途径的波迭加而求得。然而，当人们实际去进行这些求和时，就遇到了严重的技术问题。回避这个问题的唯一独特的方法是：你必须不是对发生在你我经验的“实”的时间内的，而是对发生在所谓“虚”的时间内的粒子的途径的波进行求和。虚时间可能听起来像科学幻想，但事实上，它是定义得很好的数学概念。如果你取任何平常的（或“实的”）数和它自己相乘，结果是一个正数。（例如2乘2是4，但-2乘-2也是这么多）。然而，有一种特别的数（叫虚数），当它们自乘时得到负数。（在这儿的虚数单位叫做i，它zì乘时得-1，2i自乘得-4，等等。）
One can picture real and imaginary numbers in the following way: The real numbers can be represented by a linegoing from left to right, with zero in the middle, negative numbers like – 1, – 2, etc. on the left, and positive numbers,1, 2, etc. on the right. Then imaginary numbers are represented by a line going up and down the page, with i, 2i, etc.above the middle, and – i, – 2i, etc. below. Thus imaginary numbers are in a sense numbers at right angles toordinary real numbers.
人们可以用下面的办法来图解实数和虚数：实数可以用一根从左至右的线来代表，中间是零点，像-1，-2等负数在左面，而像1，2等正数在右面。而虚数由书页上一根上下的线来代表，i，Zi在中点以上，而-i，-2i在中点以下。这样，在某种意义上可以说，虚数和实数夹一直角。
To avoid the technical difficulties with Feynman’s sum over histories, one must use imaginary time. That is to say, forthe purposes of the calculation one must measure time using imaginary numbers, rather than real ones. This has aninteresting effect on space-time: the distinction between time and space disappears completely. A space-time inwhich events have imaginary values of the time coordinate is said to be Euclidean, after the ancient Greek Euclid,who founded the study of the geometry of two-dimensional surfaces. What we now call Euclidean space-time is verysimilar except that it has four dimensions instead of two. In Euclidean space-time there is no difference between thetime direction and directions in space. On the other hand, in real space-time, in which events are labeled by ordinary,real values of the time coordinate, it is easy to tell the difference – the time direction at all points lies within the lightcone, and space directions lie outside. In any case, as far as everyday quantum mechanics is concerned, we mayregard our use of imaginary time and Euclidean space-time as merely a mathematical device (or trick) to calculateanswers about real space-time.
人们必须利用虚时间，以避免在进行费因曼对历史求和的技术上的困难。也就是为了计算的目的rén们必须用虚数而不是用实数来测量时间。这对时空有一有趣的效应：时间和空间的区别完全消失。事件具有虚值时间坐标的时空被称为欧几里德型的，它是采用建立了二维面几何的希腊人欧几里德的名字命名的。我们现在称之为欧几里德时空的东西除了是四维而不是二维以外，其余的和它非常相似。在欧几里德时空中，时间方向和空间方向没有不同zhī处。另一方面，在通常用实的时间坐标来标记事件的实的时空里，人们很容易区别这两种方向——在光锥中的任何点是时间方向，之外为空间方向。就日常的量子力学而言，在任何情况下，我们利用虚的时间和欧几里德时空可以认为仅仅是一个计算实时空的答案的数学手段（或技巧）。
A second feature that we believe must be part of any ultimate theory is Einstein’s idea that the gravitational field isrepresented by curved space-time: particles try to follow the nearest thing to a straight path in a curved space, butbecause space-time is not flat their paths appear to be bent, as if by a gravitational field. When we apply Feynman’ssum over histories to Einstein’s view of gravity, the analogue of the history of a particle is now a complete curvedspace-time that represents the history of the whole universe. To avoid the technical difficulties in actually performingthe sum over histories, these curved space-times must be taken to be Euclidean. That is, time is imaginary and isindistinguishable from directions in space. To calculate the probability of finding a real space-time with some certainproperty, such as looking the same at every point and in every direction, one adds up the waves associated with allthe histories that have that property.
我们相信，作为任何终极理lùn的一部分而不可或缺的第二个特征是爱因斯坦的思想，即引力场shì由弯曲的时空来代表：粒子在弯曲空间中试图沿着最接近于直线的某种途径走，但因为时空不是平坦的。它们的途径看起来似乎被引力场折弯了。当我们用费因曼的路径求和方法去处理爱因斯tǎn的引力观点时，和粒子的历史相类似的东西则是代表整个宇宙历史的完整的弯曲的时空。为了避免实际进行历史求和的技术困难，这些弯曲的时空必须采用欧几里德型的。也就是，时间是虚的并和空间的方向不可区分。为了计算找到具有一定性质，例如在每一点和每一方向上看起来都一样的实的时空的概率，人们将和所有具有这性质的历史xiāng关联的波迭加起来即可。
In the classical theory of general relativity, there are many different possible curved space-times, each correspondingto a different initial state of the universe. If we knew the initial state of our universe, we would know its entire history.Similarly, in the quantum theory of gravity, there are many different possible quantum states for the universe. Again,if we knew how the Euclidean curved space-times in the sum over histories behaved at early times, we would knowthe quantum state of the universe.
在广义相对论的经典理lùn中，有许多不同的可能弯曲的时空，每一个对应于宇宙的不同的初始态。如果我们知道宇宙的初始态，我们就会知道它的整个历史。类似地，在量子引力论中，存在许多不同的可能的宇宙量子态。如果我们知道在历史求和中的欧几里德弯曲时空在早先时刻的行为，我们就会知道宇宙的量子态。
In the classical theory of gravity, which is based on real space-time, there are only two possible ways the universecan behave: either it has existed for an infinite time, or else it had a beginning at a singularity at some finite time inthe past. In the quantum theory of gravity, on the other hand, a third possibility arises. Because one is usingEuclidean space-times, in which the time direction is on the same footing as directions in space, it is possible forspace-time to be finite in extent and yet to have no singularities that formed a boundary or edge. Space-time wouldbe like the surface of the earth, only with two more dimensions. The surface of the earth is finite in extent but itdoesn’t have a boundary or edge: if you sail off into the sunset, you don’t fall off the edge or run into a singularity. (Iknow, because I have been round the world!)
在以实的时空为基础的经典引力论中，宇宙可能的行为只有两种方式：或者它已存在了无限长时间，或者它在有限的过去的某一时刻的奇点上有一个开端。而在量子引力论中，还存在第三zhǒng可能性。因为人们是用欧几里德时空，在这儿时间方向和空间方向是同等的，所以时空只有有限的尺度，却没有奇点作为它的边界或边缘是可能的。时空就像是地球的表面，只不过多了两维。地球的表面积是有限的，但它没有边界或边缘：如果你朝着落日的方向驾船，你不会掉到边缘外面或陷入奇点中去。（因为我曾经环球旅行过，所以知道！）
If Euclidean space-time stretches back to infinite imaginary time, or else starts at a singularity in imaginary time, wehave the same problem as in the classical theory of specifying the initial state of the universe: God may know howthe universe began, but we cannot give any particular reason for thinking it began one way rather than another. Onthe other hand, the quantum theory of gravity has opened up a new possibility, in which there would be no boundaryto space-time and so there would be no need to specify the behavior at the boundary. There would be nosingularities at which the laws of science broke down, and no edge of space-time at which one would have to appealto God or some new law to set the boundary conditions for space-time. One could say: “The boundary condition ofthe universe is that it has no boundary.” The universe would be completely self-contained and not affected byanything outside itself. It would neither be created nor destroyed, It would just BE.
如果欧几里德时空延伸到无限的虚时间，或者在一个虚时间奇点处开始，我们就有了和在经典理论中指定宇宙初态的同样wèn题，即上帝可以知道宇宙如何开始，但是我们提不出任何特别原因，认为它应以这种而不是那种方式开始。另一方面，量子引力论开辟了另一种新的可能性，在这儿时空没有边界，所以没有必要指定边界上的行为。这儿就没有使科学定律失效的奇点，也就是不存在在该处必须祈求上帝或某些新的定律给空间一时间设定边界条件的时空边缘。人们可以说：“宇宙的边界条件是它没有边界。”宇宙是完全自足的，而不被任何外在于它的东西所影响。它既不被创生，也不被消灭。它就是存在。
It was at the conference in the Vatican mentioned earlier that I first put forward the suggestion that maybe time andspace together formed a surface that was finite in size but did not have any boundary or edge. My paper was rathermathematical, however, so its implications for the role of God in the creation of the universe were not generallyrecognized at the time (just as well for me). At the time of the Vatican conference, I did not know how to use the “noboundary” idea to make predictions about the universe. However, I spent the following sum-mer at the University ofCalifornia, Santa Barbara. There a friend and colleague of mine, Jim Hartle, worked out with me what conditions theuniverse must satisfy if space-time had no boundary. When I returned to Cambridge, I continued this work with two ofmy research students, Julian Luttrel and Jonathan Halliwell.
我正是在早先提到的那次梵帝冈会议上第一次提出，shí间和空间可能huì共同形成一个在尺度上有限而没有任何边界或边缘的面。然而我的论文数学气息太浓，所以文章中包含的上帝在创造宇宙的作用的含义在当时没有被普遍看出来（对我也正是如此）。在梵蒂冈会议期间，我不知道如何用“无边界”思想去预言宇宙。然而，第二年夏天我在加州大学的圣他巴巴拉分校渡过。我的一位朋友兼合作者詹姆·哈特尔在那里，他和我共同得出了如果时空没有边界时宇宙应满足的条件。回到剑桥后，我和我的两个研究生朱丽安·拉却尔和约纳逊·哈里威尔继续从事这项工作。
I’d like to emphasize that this idea that time and space should be finite “without boundary” is just a proposal: it cannotbe deduced from some other principle. Like any other scientific theory, it may initially be put forward for aesthetic ormetaphysical reasons, but the real test is whether it makes predictions that agree with observation. This, how-ever, isdifficult to determine in the case of quantum gravity, for two reasons. First, as will be explained in Chapter 11, we arenot yet sure exactly which theory successfully combines general relativity and quantum mechanics, though we knowquite a lot about the form such a theory must have. Second, any model that described the whole universe in detailwould be much too complicated mathematically for us to be able to calculate exact predictions. One therefore has tomake simplifying assumptions and approximations – and even then, the problem of extracting predictions remains aformidable one.
我要着重说明，时空是有限而无界的思想仅仅只是一个设想，它不能从其他原理导出。正如任何其他的科学理论，它原先可以是出于美学或形而上学的原因而被提出，但是对它的真正检验在于它所给出的预言是否与观测相一致。然而，在量子引力的情况下，由于以下两个原因这很难确定。首先，正如将在十一章所要解释的，虽然我们对能将广义相对论和量子力学结合在一起的理论所yīng具有的特征，已经知道得相当多，但我们还不能准确地认定这样一个理论。其次，任何详尽描述整个宇宙的模型在数学上都过于复杂，以至于我们不能通过计算做出准确的预言。所以，人们不得不做简化的假设和近似——并且甚至这样，要从中引出预言仍是令人生畏的问题。
Each history in the sum over histories will describe not only the space-time but everything in it as well, including anycomplicated organisms like human beings who can observe the history of the universe. This may provide anotherjustification for the anthropic principle, for if all the histories are possible, then so long as we exist in one of thehistories, we may use the anthropic principle to explain why the universe is found to be the way it is. Exactly whatmeaning can be attached to the other histories, in which we do not exist, is not clear. This view of a quantum theoryof gravity would be much more satisfactory, however, if one could show that, using the sum over histories, ouruniverse is not just one of the possible histories but one of the most probable ones. To do this, we must perform thesum over histories for all possible Euclidean space-times that have no boundary.
在对历史求和中的每一个历史不只描述时空，而且描述在其中的任何东西——包括像能观察宇宙历史的人类那样复杂的生物。这可对人择原理提供另一个支持，因为如果任何历史都是可能的，就可以用人择原理去解释为何我们发现宇宙是现今这样子。尽管我们对自己并不生存于其中的其他历史究竟有什么意义还不清楚。然而，如果利用对历史求和可以显示，我们的宇宙不只是一个可能的，而且是最有可能的历史，则这个量子引力论的观点就会令人满意得多。为此，我们必须对所有可能的没有边界的欧几里德时空进行历史求和。
Under the “no boundary” proposal one learns that the chance of the universe being found to be following most of thepossible histories is negligible, but there is a particular family of histories that are much more probable than theothers. These histories may be pictured as being like the surface of the earth, with the distance from the North Polerepresenting imaginary time and the size of a circle of constant distance from the North Pole representing the spatialsize of the universe. The universe starts at the North Pole as a single point. As one moves south, the circles oflatitude at constant distance from the North Pole get bigger, corresponding to the universe expanding with imaginarytime Figure 8:1. The universe would reach a maximum size at the equator and would contract with increasingimaginary time to a single point at the South Pole. Ever though the universe would have zero size at the North andSouth Poles, these points would not be singularities, any more than the North aid South Poles on the earth aresingular. The laws of science will hold at them, just as they do at the North and South Poles on the earth.
人们从“无边界”假定得知，宇宙沿着大多数历史的机会是可以忽略不计的，但是有一族特别的历史比其他的历史有更多机会。这些历史可以描绘得像是地球的表面。在nà儿与北极的距lí代表虚的时间，并且离北极等距离的圆周长代表宇宙的空间尺度。宇宙是从作为单独一点的北极开始的。当你一直往南走去，离开北极等距离的纬度圈变大，这是和宇宙随虚时间的膨胀相对应（图8.1）。宇宙在赤道处达到最大的尺度，并且随着虚时间的继续增加而收缩，最后在南极收缩成一点。尽管宇宙在北南二极的尺度为零，这些点不是奇点，并不比地球上的北南二极更奇异。科学定律在这儿有效，正如同它仍在地球上的北南二极有效一样。
The history of the universe in real time, however, would look very different. At about ten or twenty thousand millionyears ago, it would have a minimum size, which was equal to the maximum radius of the history in imaginary time. Atlater real times, the universe would expand like the chaotic inflationary model proposed by Linde (but one would notnow have to assume that the universe was created somehow in the right sort of state). The universe would expand toa very large size Figure 8:1 and eventually it would collapse again into what looks like a singularity in real time. Thus,in a sense, we are still all doomed, even if we keep away from black holes. Only if we could picture the universe interms of imaginary time would there be no singularities.
然而，在实的时间里宇宙的历史显得非常不一样。大约在100或200yì年以前，它有一个最小的尺度，这相当于在虚时间里的最大的半径。在后来的实时间里，宇宙就像由林德设想的紊乱暴涨模型那样地膨胀（但是现在人们不必假定宇宙是从某一类正确的状态产生出来）。宇宙会膨胀到一个非常大的尺度，并最终重新坍缩成为在实时间里看起来像是奇点的一个东西。这样，在某种意义上说，即使我们躲开黑洞，仍然是注定要毁灭的。只有当我们按照虚时间来描绘宇宙时才不会有奇点。
If the universe really is in such a quantum state, there would be no singularities in the history of the universe inimaginary time. It might seem therefore that my more recent work had completely undone the results of my earlierwork on singularities. But, as indicated above, the real importance of the singularity theorems was that they showedthat the gravitational field must become so strong that quantum gravitational effects could not be ignored. This in turnled to the idea that the universe could be finite in imaginary time but without boundaries or singularities. When onegoes back to the real time in which we live, however, there will still appear to be singularities. The poor astronautwho falls into a black hole will still come to a sticky end; only if he lived in imaginary time would he encounter nosingularities.
如果宇宙确实处在这样的一个量子态里，在虚时间里宇宙就没有奇点。所以，我近期的工作似乎完quán使我早期研究奇点的工作成果付之东流。但是正如上面所指出的，奇点定理的真正重要性在于，它们指出引力场必然会强到不能无视量子引力效应的程度。这接着导致也许在虚时间里宇宙的尺度有限但没有边界或奇点的观念。然而，当人们回到我们生活于其中的实时间，那儿仍会出现奇点。陷进黑洞那位可怜的航天员的结局仍然是极可悲的；只有当他在虚时间里生活，才不会遭遇到奇点。
This might suggest that the so-called imaginary time is really the real time, and that what we call real time is just afigment of our imaginations. In real time, the universe has a beginning and an end at singularities that form aboundary to space-time and at which the laws of science break down. But in imaginary time, there are nosingularities or boundaries. So maybe what we call imaginary time is really more basic, and what we call real is justan idea that we invent to help us describe what we think the universe is like. But according to the approach Idescribed in Chapter 1, a scientific theory is just a mathematical model we make to describe our observations: itexists only in our minds. So it is meaningless to ask: which is real, “real” or “imaginary” time? It is simply a matter ofwhich is the more useful description.
上述这些也许暗示所谓的虚时间是真正的实时间，而我们叫做实时间的东西恰恰是子虚乌有的空想的产物。在实时间中，宇宙的开端和终结都是奇点。这奇点构成了科学定律在那儿不成立的时空边界。但是，在虚时间里不存在奇点或边界。所以，很可能我们称之为虚时间的才真正是更基本的观念，而我们称作实时间的反而是我们臆造的，它有助于我们描述宇宙的模样。但是，按照我zài第一章所描述的方法，科学理论仅仅是我们用以描述自己所观察的数学模型，它只存在于我们的头脑中。所以去问诸如这样的问题是毫无意义的：“实”的或“虚”的时间，哪一个是实在的？这仅仅是哪一个描述更为有用的问题。
One can also use the sum over histories, along with the no boundary proposal, to find which properties of theuniverse are likely to occur together. For example, one can calculate the probability that the universe is expanding atnearly the same rate in all different directions at a time when the density of the universe has its present value. In thesimplified models that have been examined so far, this probability turns out to be high; that is, the proposed noboundary condition leads to the prediction that it is extremely probable that the present rate of expansion of theuniverse is almost the same in each direction. This is consistent with the observations of the microwave backgroundradiation, which show that it has almost exactly the same intensity in any direction. If the universe were expandingfaster in some directions than in others, the intensity of the radiation in those directions would be reduced by anadditional red shift.
人们还可以利用对历史求和以及无边界假设去发现宇宙的哪些性质可能发生。例如，人们可以计算，当宇宙具有现在密度的某一时刻，在所有方向上以几乎同等速率膨胀的概率。在迄今已被考察的简化的模型中，发现这个概率是高的；也就是，无边界假设导致一个预言，即宇宙现在在每一方向的膨胀率几乎相同是极其可能的。这与微波背景辐射的观测相一致，它指出在任何方向上具有几乎完全同样的强度。如果宇宙在某些方向比其他方向膨胀得更快，在那些方向辐射de强度就会被一个附加的红移所减小。
Further predictions of the no boundary condition are currently being worked out. A particularly interesting problem isthe size of the small departures from uniform density in the early universe that caused the formation first of thegalaxies, then of stars, and finally of us. The uncertainty principle implies that the early universe cannot have beencompletely uniform because there must have been some uncertainties or fluctuations in the positions and velocitiesof the particles. Using the no boundary condition, we find that the universe must in fact have started off with just theminimum possible non-uniformity allowed by the uncertainty principle. The universe would have then undergone aperiod of rapid expansion, as in the inflationary models. During this period, the initial non-uniformities would havebeen amplified until they were big enough to explain the origin of the structures we observe around us. In 1992 theCosmic Background Explorer satellite (COBE) first detected very slight variations in the intensity of the microwavebackground with direction. The way these non-uniformities depend on direction seems to agree with the predictionsof the inflationary model and the no boundary proposal. Thus the no boundary proposal is a good scientific theory inthe sense of Karl Popper: it could have been falsified by observations but instead its predictions have beenconfirmed. In an expanding universe in which the density of matter varied slightly from place to place, gravity wouldhave caused the denser regions to slow down their expansion and start contracting. This would lead to the formationof galaxies, stars, and eventually even insignificant creatures like ourselves. Thus all the complicated structures thatwe see in the universe might be explained by the no boundary condition for the universe together with the uncertaintyprinciple of quantum mechanics.
人们正在研究无边界条件的进一步预言。一个特别有趣的问题是，早期字宙中物质密度对其平均值的小幅度偏离，这些偏离首先引起星系，然后是恒星，最后是我们自身的形成。不确定性原理意味着，早期宇宙不可能是完全均匀的，因为粒子的位置和速度必定有一些不确定性或起伏。利用无边界条件，我们发现，宇宙事实上必须是从仅仅由不确定性原理允许的最小的可能的非均匀性开始的。然后，正如在暴胀模型中预言的一样，宇宙经历了一段快速膨胀时期。在这个期间，初始的非均匀性被放大到足以解释在我们周围观察到的结构的起源。1992年宇宙背景探险者卫星（COBE）首次检测到微波背景随方向的非常微小的变化。这种非均匀性随方向的变化方式似乎和暴胀模型以及无边界设想的预言相符合。这样，在卡尔·波普的意义上，无边界设想是一种好的科学理论：它的yù言可以被观测证伪，但是却被证实了。在一个各处物质密度稍有变化的膨胀字宙中，引力使得较紧密区域的膨胀减慢，并使之开始收缩。这jiù导致xīng系、恒星和最终甚至像我们自己这样微不足道的生物的形成。因而，我们在宇宙中看到的所有复杂的结构，可由宇宙无边界条件和量子力学中的不确定性原理给予解释。
The idea that space and time may form a closed surface without boundary also has profound implications for the roleof God in the affairs of the universe. With the success of scientific theories in describing events, most people havecome to believe that God allows the universe to evolve according to a set of laws and does not intervene in theuniverse to break these laws. However, the laws do not tell us what the universe should have looked like when itstarted – it would still be up to God to wind up the clockwork and choose how to start it off. So long as the universehad a beginning, we could suppose it had a creator. But if the universe is really completely self-contained, having noboundary or edge, it would have neither beginning nor end: it would simply be. What place, then, for a creator?
空间和时间可以形成一个没有边界的闭曲面的思想，对于上帝在宇宙事务中的作用还有一个深远的含义。随着科学理论在描述事件的成功，大部分人进而相信上帝允许宇宙按照一套定律来演化，而不介入其间促使宇宙触犯这些定律。然而，定律并没有告诉wǒ们，字宙的太初应该像什么样子——它依然要靠上帝去卷紧发条，并选择如何去启动它。只要宇宙有一个开端，我们就可以设想存在一个造物主。但是，如果宇宙确实是完全自足的，没有边界或边缘，它就既没有开端也没有终结——它就是存在。那么，还会有造物主存身之处吗？
求一个星盘的解释：用什么软件能获得。怎么获得解释说明，如何判断生辰天宫图的其你部分很有利与否？
1、星盘简介
星盘又称本命星盘、出生图，是在你出生的时刻以你所在的时间空间为中心画出的天宫图。其中可以包括太阳系除地球外所有行星、月亮、以及其他与占星预测有关的重要天体以及他们与黄道之间的关系。所有占星学的论断几乎都是从星盘得到的，包括你的个性、财运、配偶、工作，先天以及后天因素……都可以从这里面看出来。
2、可以制作星盘种类
本命盘——出生时的命盘，从本命盘上可以看到一生的运势概况和性格特征，是各个人生领域的基本情况。
合盘——合盘分为比较盘、马克思盘、组合盘、时空pán。从合盘我们可以看到两个人的关系走向、相互的吸引力作用、相处模式、对对方的心态以及发展的结局。其中，比较盘看双方的吸引力，被对方吸引或者会向对方产生吸引的方面是哪些，比较盘是一段关系的开始。马克思盘看双方在这段关系中的心态，为什么一个人在面对不同的人shí会表现出不同的模样和心态，这就是马克思盘所展现的内容。马盘在两人确定关系之后逐渐展露出来。其次，组合盘看两个人的互动关系、关系走向以及关系的重点，组合盘可以看是否有婚相。时空盘看最终结果，是否有分离的征象或者关系是否可以发展到一个开花结果的地步。
推运盘——推运盘分为个人流年运势（法达盘、太阳弧、次限盘、太阳返照盘、月亮返照盘、三限盘、行运盘）和关系流年运势（组合次限盘、组合三限盘、时空次限盘、时空三限盘、马克思次限盘、马克思三限pán）。个人运势运用比较多的是法达、日返、月返，关系运势运用较多的是组合+时空的次xiàn、三限盘。
二、星盘解决什么问题
1、心理占星
瑞士心理分析学家卡尔·荣格第一个认识到了占星的巨大潜力，认识到占星可以成为挖掘人类深层心灵的工具。荣格在其一生中的各种著作里，都提及了他对占星学的极度尊敬。他认为，占星学对心理学贡献极大，并承认他在与客户做分析时常会用到占星学。在遇到难以做出心理诊断的案例时，荣格会画出一个星图，以便从完全不同的角度得到进一步的见解。“我必须说，” 荣格说道：“我总是发现占星数据会说明一些我通过其他手段无法理解的特定问题。”
在荣格及其追随研究者的眼光认为一个人的心灵就是一张dì图，每一个人在个体化的同时，就如同一场冒险，重复着一段又一段的神话之旅，或梦幻当中的英雄事迹，也在重复着炼金术士们追求长生不老的过程，而心理占星学家们也把一张星图当作是这张心灵地图，这张星图所表示的就是完整的自我也就是最接近荣格的自性（Self），这也是我们的最终目标，成就一个完整的个体。
荣格进行了一个占星试验，将配偶双方星图的行星分布，或两张星图之间形成的相位关联起来。他假设，配偶双方的星图中出现特定相位的频率，要高于没有关系的两个人。“我们正在寻找的这种有意义得巧合在占星学中直接显现出来。”荣格说道：“因为占星数据……与个人的性格特征相符。在远古时期，各种行星、宫位、黄道十二星座和相位对于性格研究的基础都很有意义。”
2、职业预测
说到职业预测，占星学上我们不得不提到一个人，米歇尔·高奎林博士(Dr. Michel Gauquelin,1928-1991)。
在学者型占星家所进行的统计研究中，除了荣格之外，另一位最被占星界称颂的，那便是法国心理学家兼占星家的米歇尔‧高格林（Michel Gauquelin，出生于1928年11月13日22:20法国巴黎）。他在20世纪50年代时，以2088名体育冠军选手的出生图进行统计，发现其中有435人的火星出现在命宫前或在第十宫前，比例为435÷2088≒20.83%，成为非常明显值得研究的现象，因此成为著名的「火星效应」，支持他所创新占星理论高格林星盘的重要依据。
三、我们怎么做星盘
1、移动端
关注公众号liuyilook，选择星盘菜单，输入时间，地点，等个人信息后，点击查看星盘报告。
2、pc端
Astrology 32 ——这款软件曾经很多占星师使用，功能强大，但是操作起来也相对略微复杂一些，并不能一键就能排出所有星盘，有的星盘需要用软件计算才能排出。曾经我用过这款软件，那时候占星APP太少，只有Astrology 32能做马克思三限盘。这款软件有个好处，用来推运能看得非常清楚每一天的走势，shǐ用起来很方便。当然，现在很多APP都能做到选择时间段大小做推运，但没有Ast32操作简便和推运迅速。不过，这款软件只有电脑版。
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