Omega, Camille Flammarion [top 10 books to read TXT] 📗

one even remember to have ever taken any interest in them? The courts themselves had no cases; one does not murder when one expects the end of the world. Humanity no longer attached importance to anything; its heart beat furiously, as if about to stop forever. Every face was emaciated, every countenance discomposed, and haggard with sleeplessness. Feminine coquetry alone held out, but in a superficial, hesitating, furtive manner, without thought of the morrow.

The situation was indeed serious, almost desperate, even in the eyes of the most stoical. Never, in the whole course of history had the race of Adam found itself face to face with such a peril. The portents of the sky confronted it unceasingly with a question of life and death.

But, let us go back to the beginning.

Three months before the day of which we speak, the director of the observatory of Mount Gaurisankar had sent the following telephonic message to the principal observatories of the globe, and especially to that of Paris:1

“A telescopic comet discovered tonight, in 290°, 15′ right ascension, and 21°, 54′ south declination. Slight diurnal motion. Is of greenish hue.”

Not a month passed without the discovery of telescopic comets, and their announcement to the various observatories, especially since the installation of intrepid astronomers in Asia on the lofty peaks of Gaurisankar, Dapsang and Kanchinjinga; in South America, on Aconcagua, Illampon and Chimborazo, as also in Africa on Kilimanjaro, and in Europe on Elburz and Mont Blanc. This announcement, therefore, had not excited more comment among astronomers than any other of a like nature which they were constantly receiving. A large number of observers had sought the comet in the position indicated, and had carefully followed its motion. Their observations had been published in the Neuastronomischenachrichten, and a German mathematician had calculated a provisional orbit and ephemeris.

Scarcely had this orbit and ephemeris been published, when a Japanese scientist made a very remarkable suggestion. According to these calculations, the comet was approaching the Sun from infinite space in a plane but slightly inclined to that of the ecliptic, an extremely rare occurrence, and, moreover, would traverse the orbit of Saturn. “It would be exceedingly interesting,” he remarked, “to multiply observations and revise the calculation of the orbit, with a view to determining whether the comet will come in collision with the rings of Saturn; for this planet will be exactly at that point of its path intersected by the orbit of the comet, on the day of the latter’s arrival.”

A young laureate of the Institute, a candidate for the directorship for the observatory, acting at once on this suggestion, had installed herself at the telephone office in order to capture on the wing every message. In less than ten days she had intercepted more than one hundred despatches, and, without losing an instant, had devoted three nights and days to a revision of the orbit as based on this entire series of observations. The result proved that the German computor had committed an error in determining the perihelion distance and that the inference drawn by the Japanese astronomer was inexact in so far as the date of the comet’s passage through the plane of the ecliptic was concerned, this date being five or six days earlier than that first announced; but the interest in the problem increased, for the minimum distance of the comet from the Earth seemed now less than the Japanese calculator had thought possible. Setting aside for the moment, the question of a collision, it was hoped that the enormous perturbation which would result from the attraction of the Earth and Moon would afford a new method of determining with exhaustive precision the mass of both these bodies, and perhaps even throw important light upon the density of the Earth’s interior. It was, indeed, established that the celestial visitor was moving in a plane nearly coincident with that of the ecliptic, and would pass near the system of Saturn, whose attraction would probably modify to a sensible degree the primitive parabolic orbit, bringing it nearer to the belated planet. But the comet, after traversing the orbits of Jupiter and of Mars, was then to enter exactly that described annually by the Earth about the Sun. The interest of astronomers was not on this account any the less keen, and the young computor insisted more forcibly than ever upon the importance of numerous and exact observations.

It was at the observatory of Gaurisankar especially that the study of the comet’s elements was prosecuted. On this highest elevation of the globe, at an altitude of 8000 meters, among eternal snows which, by newly discovered processes of electrochemistry, were kept at a distance of several kilometers from the station, towering almost always many hundred meters above the highest clouds, in a pure and rarified atmosphere, the visual power of both the eye and the telescope was increased a hundred fold. The craters of the Moon, the satellites of Jupiter, and the phases of Venus could be readily distinguished by the naked eye. For nine or ten generations several families of astronomers had lived upon this Asiatic summit, and had gradually become accustomed to its rare atmosphere. The firstcomers had succumbed; but science and industry had succeeded in modifying the rigors of the temperature by the storage of solar heat, and acclimatization slowly took place; as in former times, at Quito and Bogota, where, in the eighteenth and nineteenth centuries, a contented population lived in plenty, and young women might be seen dancing all night long without fatigue; whereas on Mont Blanc in Europe, at the same elevation, a few steps only were attended with painful respiration. By degrees a small colony was installed upon the slopes of the Himalayas, and, through their researches and discoveries, the observatory had acquired the reputation of being the first in the world. Its principal instrument was the celebrated equatorial of one hundred meters focal length, by whose aid the hieroglyphic signals, addressed in vain for several