The Astrophysical journal . h all facilities for centering and adjusting plates, permits the obser-vations to be made in a most satisfactory manner. It should be stated,however, that some observers see the flocculi as apparent depressions-rather than as elevations. This, however, is uncommon. It seems probable that further studies of this character will bringuseful results. It has already been possible to detect in this waylinear markings on the solar surface, of great extent, which do notreadily strike the eye when plates are examined singly. For purposes-of measurement, and the detection of
The Astrophysical journal . h all facilities for centering and adjusting plates, permits the obser-vations to be made in a most satisfactory manner. It should be stated,however, that some observers see the flocculi as apparent depressions-rather than as elevations. This, however, is uncommon. It seems probable that further studies of this character will bringuseful results. It has already been possible to detect in this waylinear markings on the solar surface, of great extent, which do notreadily strike the eye when plates are examined singly. For purposes-of measurement, and the detection of minute differences of form,,the monocular eyepiece, with micrometer attachment, which is fur-nished by Zeiss as an accessory of the stereocomparator, is of course tobe employed. It nevertheless appears probable that the stereoscopicmethod will prove to have certain advantages of its own, which willrecommend it to those who are engaged in the study of spectrohelio-graph , 1907 X X en P w opa H < <J zp w a H. ORBIT OF THE SPECTROSCOPIC BINARY k CANCRI By NAOZO ICHINOHE This star (a = 9h2m, S= + ii°4; Mag. H. P., ; D. C, ;P. ZX, ) was found as a spectroscopic binary at Yerkes Obser-vatory by Messrs. Frost and Adams, in the course of the regularprogramme of work on stars having spectra of the Orion type. Theirmeasures of the first five plates taken (IB 256, 267, 286, 289, 305)will be found in their At the suggestion of Mr. Frost, Ibegan last summer to measure the spectrograms of the star takenlater than the above plates. The spectrum of this star belongs to the later stage of develop-ment from the Orion type toward the Sirian type. The hvdrogenlines are strong and well defined. The helium lines XX 4009, 4026,4144, 4388, and 4472 are scarcely visible. The carbon line X 4267is weli! seen; the silicon lines AA4128 and 4131 are very good formeasurement, as they are quite strong and well defined. The Kline is sharp and strong, and the magnesium line X
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Keywords: ., bookcentury1800, bookdecade1890, booksubjectspectru, bookyear1895
