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84 put forth that it was a reappearance of the long-lost comet of Lexell of 1770. Unfortunately the period and the position of the orbit are such that no return favourable for observation can be expected before 1931; and it is doubtful whether the observations of 1895 were sufficiently complete to enable the character of the orbit to be determined with precision. The period assigned by Schulhof is 7⋅19 years.

On March 26, 1894, Denning discovered in Leo Minor a faint comet which was becoming fainter because the perihelion passage had occurred as far back as Feb. 9, and the comet was receding both from the Sun and the Earth. That its orbit was elliptic, with a period of about 7$1⁄2$ years, was soon ascertained, but owing to the lack of an adequate number of observations definitive elements could not be assured. Schulhof called attention to the fact that the point of nearest approach between the orbits of the comet and Jupiter coincided very nearly with the point at which Brorsen's Comet and Jupiter were nearest one another. This fact was further emphasised by Hind, who showed that the two comets were actually very near one another 13 years previously, namely in April 1881.

This comet awaits further consideration before it can be regarded as a recognised short-period comet. Although expected to return in 1901 it was not seen in that year. Nor in 1909 thus far.

On Nov. 14, 1906, J. Metcalf at Taunton, Mass., U.S., discovered a very faint comet shining as a 12 th mag. star. It proved to be revolving in an elliptic orbit with a period of rather more than 7 years; and to be one of the Jupiter family of comets. Though the elements resemble those of the comets of Faye, Wolf, 1892 (v.), 1896 (v.), and 1900 (iii.), identity with any of these is not possible.