Abstract
ALGOL.—The periodic variations in the intervals between the minima of Algol have been explained by Dr. Chandler by supposing that the bright star, with its eclipsing companion, revolves round a distant centre of gravity determined by its relation to another dark body. M. Tisserand, however, considers that the phenomena may be produced by the changes in the line of apsides due to a polar compression of Algol (NATURE, vol. li. p. 328). The latter hypothesis requires that considerable variations in the duration of the minima should be observed; while, on Dr. Chandler's hypothesis, there should be a periodic inequality of the proper motion of Algol. Prof. Lewis Boss has recently discussed the question from the point of view of the proper motion of the star; but since the coefficient is probably less than 0″˙7, the investigation is a very delicate one. Taking the result of his computation, apart from any considerations of the behaviour of Algol as a variable star, Prof. Boss is of opinion that there is a preponderance of probability in favour of the real existence of a periodic element in the proper motion, such as is required by Dr. Chandler's hypothesis. Supposing them to be real, they indicate that the apparent motion is in an ellipse, the semi-axis major of which is 0″˙522 ± 0″˙103 and the semi-axis minor 0″˙224; the position angle of the northern end of the major axis is 34°, and the inclination of the real orbit to our line of sight is 23°. The computation further indicates that the star passed the major axis of the apparent orbit within three or four years of the most probable date derived from the observated light-changes. Prof. Boss considers the evidence in favour of Dr. Chandler's hypothesis to be sufficient to justify a very thorough investigation of the meridian observations, as well as continued determinations of position. (Astronomical Journal, No. 343.)
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Our Astronomical Column. Nature 52, 61–62 (1895). https://doi.org/10.1038/052061a0
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DOI: https://doi.org/10.1038/052061a0