The Astrophysical journal . z2 = — 675osq. mm /,= 4d76o, /2 = 7d; The following elements wereU e = derived: = 6d393= 8i° 162° 15:8= 56?3i or log/* = = T- = 1904 Jan. 6 .897 a sin i- = 5,890,000 km In order to see if the elements satisfactorily represent the obser-vations, an ephemeris was calculated; the computed values will befound in the sixth column of the above table. The last column ofthe same table gives the residuals, observation minus residuals are pretty large, ranging from + 7 km to — 7 km, butthey may be regarded as fairly satisfactory, since all
The Astrophysical journal . z2 = — 675osq. mm /,= 4d76o, /2 = 7d; The following elements wereU e = derived: = 6d393= 8i° 162° 15:8= 56?3i or log/* = = T- = 1904 Jan. 6 .897 a sin i- = 5,890,000 km In order to see if the elements satisfactorily represent the obser-vations, an ephemeris was calculated; the computed values will befound in the sixth column of the above table. The last column ofthe same table gives the residuals, observation minus residuals are pretty large, ranging from + 7 km to — 7 km, butthey may be regarded as fairly satisfactory, since all these plates ORBIT OF k CAXCRI 3T9 were taken with one prism. The mean error of a single plate is± km. There is no appreciable evidence of systematic errorsin the residuals. I did not trv to correct the elements further, as the observationaldata are not yet adequate for the calculation of the definitive accompanying figure shows the computed curve and observedpoints. +100 km + 80 + 60 + 40 + 20 -40 -60 k. I 2 3 4 5 6 7 8<i Computed Velocity-Curve for k Cancri, with Observed Points The above relates exclusively to the principal component of thespectrum of k Cancri; but the star shows another spectrum, aswas pointed out by Frost and Adams. I was able to see the faintcomponent of the spectrum on eighteen plates out of lines are so extremely faint that it is very difficult to measurethem, and the results are liable to great errors. The discussion ofthe orbit of the fainter component is therefore deferred until addi-tional plates can be obtained and greater certainty assured. Yerkes ObservatoryMay, 1907 ORBIT OF THE SPECTROSCOPIC BINARY /3 ARIETIS1 By H. LUDEXDORFF The variability of the radial velocity of /3 Arietis was announcedin 1903 by Director Vogel2 as a result of his measurements of 14spectrograms obtained by Messrs. Eberhard and Scholz and myselfwith spectrograph IV (three prisms) attached to the photo-graphic refractor of th
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Keywords: ., bookcentury1800, bookdecade1890, booksubjectspectru, bookyear1895
