Eureka: A Prose Poem — Edgar A. Poe, 1848 — reading text

be a class of superior intelligences, to whom the human bias alluded to may wear all the character of monomania. My question, however, remains unanswered : — Have we any right to infer — let us say, rather, to imagine — an inter minable succession of the" " clusters of clusters," or of " Uni verses " more or less similar ? I reply that the " right," in a case such as this, depends absolutely upon the hardihood of that imagination which ventures to claim the right. Let me declare, only, that, as an individual, I myself feel impelled to the fancy — without daring to call it more — that there does exist a limitless suc cession of Universes, more or less similar to that of which we have cognizance — to that of which alone we shall ever THE UNIVERSE. 103 have cognizance — at the very least until the return of our own particular Universe into Unity. If such clusters of clusters exist, however — and they do — it is abundantly clear that, having had no part in our origin, they have no portion in our laws. They neither attract us, nor we them. Their material — their spirit is not ours — is not that which obtains in any part of our Universe. They could not impress our senses or our souls. Among them and us — considering all, for the moment, collectively — there are no influences in common. Each exists, apart and independently, in the bo som of its proper and particular God. In the conduct of this Discourse, I am aiming less at physical than at metaphysical order. The clearness with which even material phsenomena are presented to the under standing, depends very little, I have long since learned to perceive, upon a merely natural, and almost altogether upon a moral, arrangement. If then I seem to step somewhat too discursively from point to point of my topic, let me suggest that I do so in the hope of thus the better keeping unbroken that chain of graduated impression by which alone the in tellect of Man can expect to encompass the grandeurs of which I speak, and, in their majestic totality, to comprehend them. 80 far, our attention has been directed, almost exclu sively, to a general and relative grouping of the stellar bodies in space. Of specification there has been little ; and whatever ideas of quantity have been conveyed — that is to say, of number, magnitude, and distance — have been conveyed incidentally and by way of preparation for more definitive conceptions. These latter let us now attempt to entertain. 104 EUREKA. Our solar system, as has been already mentioned, con sists, in chief, of one sun and sixteen planets certainly, but in all probability a few others, revolving around it as a centre, and attended by seventeen moons of which we know, with possibly several more of which as yet we know nothing. These various bodies are not true spheres, but oblate spheroids — spheres flattened at the poles of the ima ginary axes about which they rotate : — the flattening being a consequence of the rotation. Neither is the Sun abso lutely the centre of the system ; for this Sun itself, with all the planets, revolves about a perpetually shifting point of space, which is the system's general centre of gravity. Neither are we to consider the paths through which these different spheroids move — the moons about the planets, the planets about the Sun, or the Sun about the common cen tre — as circles in an accurate sense. They are, in fact, ellipses — one of the foci being the point about which the revolution is made. An ellipse is a curve, returning into itself, one of whose diameters is longer than the other. In the longer diameter are two points, equidistant from the middle of the line, and so situated otherwise that if, from each of them a straight line be drawn to any one point of the curve, the two lines, taken together, wrill be equal to the longer diameter itself. Now let us conceive such an ellipse. At one of the points mentioned, which are the foci, let us fasten an orange. By an elastic thread let us connect this orange with a pea ; and let us place this latter on the cir cumference of the ellipse. Let us now move the pea con tinuously around the orange — keeping always on the cir cumference of the ellipse. The elastic thread, which, of THE UNIVERSE. 105 course, varies in length as we move the pea, will form what in geometry is called a radius vector. Now, if the orange be understood as the Sun, and the pea as a planet revolving about it, then the revolution should be made at such a rate — with a velocity so varying — that the radius vector may pass over equal areas of space in equal times. The pro gress of the pea should be — in other words, the progress of the planet is, of course, — slow in proportion to its distance from the Sun — swift in proportion to its proximity. Those planets, moreover, move the more slowly which are the farther from the Sun ; the squares of their periods of revo lution having the same proportion to each other, as have to each other the cubes of their mean distances from the Sun. The wonderfully complex laws of revolution here de scribed, however, are not to be understood as obtaining in our system alone. They everywhere prevail where Attrac tion prevails. They control the Universe. Every shining speck in the firmament is, no doubt, a luminous sun, resem bling our own, at least in its general features, and having in attendance upon it a greater or less number of planets, greater or less, whose still lingering luminosity is not suffi cient to render them visible to us at so vast a distance, but which, nevertheless, revolve, moon-attended, about their starry centres, in obedience to the principles just detailed — in obedience to the three omniprevalent laws of revolution — the three immortal laws guessed by the imaginative Kep ler, and but subsequently demonstrated and accounted for by the patient and mathematical Newton. Among a tribe of philosophers who pride themselves excessively upon 6* 106 EUREKA. matter-of-fact, it is far too fashionable to sneer at all specu lation under the comprehensive sobriquet, " guess-work." The point to be considered is, who guesses. In guessing with Plato, we spend our time to better purpose, now and then, than in hearkening to a demonstration by Alcmseon. In many works on Astronomy I find it distinctly stated that the laws of Kepler are the basis of the great principle, Gravitation. This idea must have arisen from the fact that the suggestion of these laws by Kepler, and his proving them a posteriori to have an actual existence, led Newton to account for them by the hypothesis of Gravitation, and, finally, to demonstrate them a priori, as necessary conse quences of the hypothetical principle. Thus so far from the laws of Kepler being the basis of Gravity, Gravity is the basis of these laws — as it is, indeed, of all the laws of the material Universe which are not referable to Repulsion alone. The mean distance of the Earth from the Moon — that is to say, from the heavenly body in our closest vicinity — is 237,000 miles. Mercury, the planet nearest the Sun, is distant from him 37 millions of miles. Venus, the next, revolves at a distance of 68 millions : — the Earth, which comes next, at a distance of 95 millions : — Mars, then, at a distance of 144 millions. Now come the eight Asteroids (Ceres, Juno, Vesta, Pallas, Astraa,. Flora, Iris, and Hebe) at an average distance of about 250 millions. Then we have Jupiter, distant 490 millions ; then Saturn, 900 mil lions ; then Uranus, 19 hundred millions ; finally Neptune; lately discovered, and revolving at a distance, say of 28 THE UNIVERSE. 107 hundred millions. Leaving Neptune out of the account — of which as yet we know little accurately and which is, possibly, one of a system of Asteroids — it will be seen that, within certain limits, there exists an order of interval among the planets. Speaking loosely, we may say that each outer planet is twice as far from the Sun as is the next inner one. May not the order here mentioned — may not the law of Bode — be deduced from consideration of the analogy suggested by me as having place between the solar discharge of rings and the mode of the atomic irra diation ? The numbers hurriedly mentioned in this summary of distance, it is folly to attempt comprehending, unless in the light of abstract arithmetical facts. They are not prac tically tangible ones. They convey no precise ideas. I have stated that Neptune, the planet farthest from the Sun, revolves about him at a distance of 28 hundred millions of miles. So far good : — I have stated a mathematical fact ; and, without comprehending it in the least, we may put it to use — mathematically. But in mentioning, even, that the Moon revolves about the Earth at the comparatively trifling distance of 237,000 miles, I entertained no expec tation of giving any one to understand — to know — to feel — how far from the Earth the Moon actually is. 237,000 miles ! There are, perhaps, few of my readers who have not crossed the Atlantic ocean ; yet how many of them have a distinct idea of even the 3,000 miles intervening between shor« and shore ? I doubt, indeed, whether the man lives who can force into his brain the most remote con ception of the interval between one milestone and its next 108 EUREKA. neighbor upon the turnpike. We are in some measure aided, however, in our consideration of distance, by com bining this consideration with the kindred one of velocity. Sound passes through 1100 feet of space in a second of time. Now were it possible for an inhabitant of the Earth to see the flash of a cannon discharged in the Moon, and to hear the report, he would have to wait, after perceiving the former, more than 13 entire days and nights before getting any intimation of the latter. However feeble be the impression, even thus conveyed, of the Moon's real distance from the Earth, it will, never theless, effect a good object in enabling us more clearly to see the futility of attempting to grasp such intervals as that of the 28 hundred millions of miles between our Sun and Neptune ; or even that of the 95 millions between the Sun and the Earth we inhabit. A cannon-ball, flying at the greatest velocity with which such a ball has ever