Our Astronomical Column

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    THE MOTION OF THE SOLAR SYSTEM.—The methods elaborated by Argelander and Airy for the numerical solution of this problem have been followed with more or less variation by a host of investigators. As a rule the deviations in method have involved matters of detail rather than any fresh departure. Various suppositions have been made as to the motions of the stars themselves (motus peculiares): that the magnitude and direction of these motions have no connection with position, or that, in general, all these motions take place with the same angular velocity parallel to the galactic circle. Stars may be grouped according to their brilliancy, or the amount of their proper motion, or they may be arranged with more or less ingenuity according to their apparent position; but when the final equations are solved, the results are found to be fairly accordant. This fact has been recently demonstrated by M. Pannekoek, who, to vary the problem as much as possible, has based his investigations on the type of spectrum presented by the star. The zone from which the stars are selected is somewhat limited, being restricted to 0°—20° of declination, the spectra of which have been observed at Potsdam. The stars have been divided into four groups, according to the amount of the proper motion, with the following results:—

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    Our Astronomical Column. Nature 52, 135–136 (1895) doi:10.1038/052135a0

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