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194 4Ap J 99. . 210S NEW ORBITS for THE 210S . 99. NEW ORBITS FOR THE SPECTROSCOPIC BINARIES HD 163181 AND HD 78316 (76 k CANCRI)* J 4Ap Otto Struve 194 McDonald and Yerkes Observatories Received November 10, 1943 ABSTRACT ED 163181.—A new orbit has been derived for this eclipsing variable from 55 McDonald Observatory- plates. The elements agree with those determined in 1928 at Mount Wilson, except that e is 0.10 instead of 0.065. The velocity-curve shows a conspicuous rotation effect at phases on both sides of 6 days—which is GaposchkhTs secondary minimum. The system consists of a very luminous B star with strong absorp- tion lines and an equally luminous star which is associated with an emitting nebulosity of B and Bei. HD 78316 (k Cancri).—A new orbit has been derived from 84 Yerkes single-prism spectrograms and 3 McDonald Cassegrain plates. The elements agree well with those recently determined at Victoria except for an unexplained difference in y and a small difference in a>. The spectrum contains unusually strong lines oí Mnu. HD 1631811 This star is of special interest because it has bright lines of variable intensity, which have sometimes been likened to the bright lines in the spectrum of ß Lyrae. A compari- son of the two stars is, however, at first quite disappointing. On the first few spectro- grams taken at the McDonald Observatory the bright lines were very weak; and, al- though on later dates they became somewhat stronger, they never even remotely re- sembled the conspicuous enfission lines of ß Lyrae. However, a more critical examination of the 55 spectrograms obtained between July 9 and September 15,1943, shows a number of very interesting features which may help in elucidating some of the puzzles which abound in our discussions of Be stars. The binary nature of HD 163181 was discovered at the Mount Wilson Observatory, and an orbit was published in 1928 by Humason and Nicholson.2 The period is almost ex- actly 12 days, and the range in velocity is 385 km/sec. The eccentricity is 0.065, and the longitude of periastron is 23.2°. Humason and Nicholson discovered the variability of the emission lines and also of the absorption lines and established the principal character- istics of these variations. Through their kindness I was able to examine several of their spectrograms. There seems to have been no appreciable change in the intensity or ap- pearance of the bright and dark lines. The star took an added importance when S. Gaposchkin,3 in 1938, announced that it is an eclipsing variable with two almost equal minima, whose depths are 0.43 and 0.42 mag., respectively. Since then the variable has also been observed by Hertzsprung4 and his as- sociates, who find a ß Lyrae-type fight-curve and closely confirm the results of Gaposch- kin. I have adopted Gaposchkin’s epoch of principal minimum, JD 2428429.79, and his period of 12.004211 days and have computed my phases with the help of these data. The radial velocities are fisted in Table 1. Separate columns give the mean results from all fines except those of interstellar calcium, from the calcium fines, and from the H fines. * Contributions from the McDonald Observatory, University of Texas, No. 86. i V453 Sco; a = Ô = -32°27' (1900), mag. 6.6, Sp. B0. *Ap. /., 67, 341, 1928. 3 Harvard Bull., No. 909, p. 20, 1938; Ap. /., 89, 125 and 322, 1939. 4 Quoted by Mrs. C. P. Gaposchkin from a letter by Professor Hertzsprung to Dr. Harlow Shapley dated December 9, 1940. 210 © American Astronomical Society • Provided by the NASA Astrophysics Data System 210S . 99. J 4Ap NEW ORBITS FOR SPECTROSCOPIC BINARIES 211 194 TABLE 1 . Radial Velocities of HD 163181 Velocities in Km/Sec Date JD 1943 U.T. 2430000+ Phase Qual No. No. No. O-C of All of Ca n of Lines Lines Lines Lines July 9. 5:48 914.74 0.08 g 14 - 72.6 - 81.0 - 2.2 9. 6:07 914.76 0.16 g 15 - 60.1 + 16.2 - 73.9 + 3.5 11. 6:22 916.77 2.11 g 15 + 111.8 + 2.1 + 108.6 - 3.1 11. 7:26 916.81 2.15 g 18 + 107.4 - 7.3 + 102.0 -10.8 12. 5:33 917.73 3.07 g 17 + 156.2 - 4.5 + 150.8 -10.3 12. 6:16 917.76 3.10 g 15 + 162.4 - 4.9 + 165.1 - 4.7 13. 5:26 918.73 4.07 g 15 + 158.0 - 0.9 + 162.0 + 5.3 13. 5:56 918.75 4.09 g 16 + 135.5 -15.0 + 140.5 -16.2 14. 5:51 919.74 5.08 v.p. 5 + 61.9 + 44.7 - 7.8 14. 6:09 919.76 5.10 g 13 + 78.0 + 3.1 + 56.7 + 10.4 18. 5:28 923.73 8.07 g 16 -217.0 - 5.3 -202.0 -22.0 22. 6:55 927.79 1.12 P 8 + 48.9 + 10.8 +22.0 22. 7:15 927.80 I. g 6 + 30.9 + 7.21 + 3.2 3 23. 6:14 928.76 2.09 g 15 + 113.3 - 6.1 +102.7 - 0.3 28. 4:32 933.69 7.02 P 2 -128.3 -170.0 + 2.9 28. 4:50 933.70 7.03 g 13 -146.1 -146.2 -13.9 29. 4:15 934.68 8.01 g 18 -196.0 -60.3 -178.2 - 3.3 Aug. 6. 2:37 942.61 3.94 g 15 +149.8 -12.0 + 166.7 - 9.0 7. 2:34 943.61 4.94 P 8 + 112.3 + 87.5 +28.2 8. 2:46 944.62 5.95 g 13 + 6.7 +10.5 - 11.4 +33.3 8. 3:06 944.63 5.96 g 15 - 8.7 + 4.2 - 5.2 + 18.9 9. 2:24 945.60 6.93 v.p. 6 -137.4 -119.2 -13.7 9. 2:39 945.61 6.94 g 8 -121.6 -112.0 + 2.9 13. 2:49 949.62 10.95 g 9 -157.7 -190.7 - 2.2 14. 3:43 950.66 II. g 21 - 77.9 - 85.89 + 0.5 9 15. 2:50 951.62 0.95 g 15 + 8.2 - 20.1 - 2.0 20. 2:53 956.62 5.95 g 10 + 1.1 + 11.7 - 0.1 +27.7 25. 2:12 961.59 10.92 g 8 -163.4 -152.5 - 6.0 25. 2:30 961.60 10.93 g 12 -177.0 -154.5 -20.4 27. 2:30 963.60 0.92 g 10 + 10.1 - 20.5 + 2.8 27. 2:54 963.62 0.94 g 14 + 3.5 - 23.2 - 5.7 28. 2:27 964.60 1.92 g 8 + 91.4 + 78.5 - 8.3 29. 2:24 965.60 2.92 g 12 + 159.5 -10.7 +155.8 - 2.4 30. 2:14 966.59 3.91 g 15 + 164.6 -38.0 +164.8 + 4.6 Sept. 4. 1:54 971.58 8.90 g 16 -208.6 + 6.4 -202.0 + 5.6 5. 4:14 972.68 10.00 g 14 -200.2 0.0 -194.2 + 0.2 5. 4:36 972.69 10.01 g * 8 -187.5 -222.9 + 12.1 6. 2:00 973.58 10.90 g 16 -169.2 + 3.1 -160.2 -10.6 6. 2:20 973.60 10.92 g 16 -169.5 -15.1 -156.8 -12.1 7. 2:03 974.59 11.91 g 17 - 87.7 + 4.0 - 89.5 - 2.5 7. 2:47 974.62 11.94 g 18 - 90.8 + 2.4 -100.8 - 8.1 8. 1:54 975.58 0.90 g 17 + 10.7 + 12.0 - 29.2 + 5.4 8. 2:15 975.59 0.91 g 16 0.6 + 18.1 - 21.3 - 6.9 8. 2:51 975.62 0.94 g 20 + 16.7 - 1.8 - 3.9 + 7.5 8. 3:26 975.64 0.96 g 17 + 9.1 - 0.3 - 9.1 - 2.2 12. 1:54 979.58 4.90 g 14 + 102.8 -15.8 +116.5 + 14.8 12. 2:16 979.59 4.91 g 15 + 95.8 - 6.8 + 98.2 + 9.0 13. 1:47 980.57 5.89 g 13 - 15.9 - 6.8 - 12.3 + 4.0. 13. 2:19 980.60 5.92 g 16 + 0.2 + 2.2 - 15.7 +23.4 13. 2:49 980.62 5.94 g 15 - 6.6 -13.0 - 12.8 +18.9 14. 1:44 981.57 6.89 g 17 -128.7 - 6.9 -142.1 - 8.1- 14. 2:17 981.60 6.92 g 16 -152.6 -16.1 -142.4 -29.5 14. 2:59 981.62 6.94 g 17 -143.3 + 2.2 -140.5 -18.8 15. 2:06 982.59 7.91 g 20 -188.9 + 2.1 -187.3 - 0.7 15. 2:30 982.60 7.92 g 13 -189.9 -198.3 - 1.3 © American Astronoihical Society • Provided by the NASA Astrophysics Data System 212 OTTO STRUVE The plates were grouped in 13 normal places as is shown in Table 2. The values of O—C are those which result from a least-squares solution. Table 3 shows a comparison of the velocities from the H lines with those from all stellar lines.
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